Cardi B Talks Motherhood And Getting Back With Offset After Cheating Scandal: ‘A Lot Of People Were So Mad At Me’
by Alyssa CroezenThis month, Vogue is celebrating powerful women who are not only creatives forces in Hollywood but are also mothers — and one of those fearless women is Cardi B.
Looking stunning on the January 2020 cover with her daughter Kulture, the “I Like It” performer gets candid with the magazine about motherhood and her relationship with Offset following his cheating scandal.
“When me and my husband got into our issues…you know, he cheated and everything and I decided to stay with him and work together with him, a lot of people were so mad at me; a lot of women felt disappointed in me,” she says.
“But it’s real-life sh**. If you love somebody and you stop being with them, and you’re depressed and social media is telling you not to talk to that person because he cheated, you’re not really happy on the inside until you have the conversation,” Cardi adds.
“Then, if you get back with them, it’s like, ‘How could you? You let all of us down.’”
Through thick and thin, the rapper admits that she and Offset are still working on their issues.
“I believe in forgiveness. I prayed on it. Me and my husband, we prayed on it. We had priests come to us,” the 27-year-old reveals.
“We just came to an understanding like, bro, it’s really us against the world. He has my back for everything, I have his back for everything, so when you cheat, you’re betraying the person that has your back the most,” Cardi continues.
“Why would you do that? We have come to a clear understanding. For me, monogamy is the only way. I’ll beat your a** if you cheat on me.”
Along with their relationship, the musical couple are also still trying to figure out how to settle into family life together with their one-year-old daughter, Kulture.
During the interview, Offset added: “It’s not an easy thing. We both have our own households.”
“But you grow. We’re way better now with communication. She’s balancing a lot. She feels like she can’t be absent a lot, and our jobs are crazy.”
“I think motherhood got her more focused. I always tell her, don’t follow the comments. But she’s been outspoken on things since before she was making music, she’s not ever putting on, she’s not ever being cool.
When it comes to motherhood, Cardi shares that “things are a little bit hard to balance.”
“It’s good for the mental. Like, if I’m playing with my daughter, I forget about the issues,” she says.
Read her full interview with Vogue here.


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Fighters
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Public Member Functions | |
| __construct (Fighter $pFighter, int $pLife) | |
| getLife () | |
| Public Member Functions inherited from Action | |
| getActor () | |
| getActionName () | |
Protected Attributes | |
| $life | |
| Protected Attributes inherited from Action | |
| $actionName | |
| $actor | |
Additional Inherited Members | |
| Protected Member Functions inherited from Action | |
| __construct (Fighter $pFighter) | |
| setActionName (string $pName) | |
Definition at line 8 of file ActionWins.php.
| __construct | ( | Fighter | $pFighter, |
| int | $pLife | ||
| ) |
constructor
| $pFighter | |
| $pLife |
Definition at line 20 of file ActionWins.php.
| getLife | ( | ) |
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protected |
Definition at line 13 of file ActionWins.php.


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To participate in this challenge you will need to sign-in on Harley-Davidson's Ride 365 website and enroll in this challenge. Be sure to read the Terms & Conditions which will provide you with information on how to submit your photos. Once these steps have been completed all that is left is to get on your Harley and hit the open road.


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Bachelor of Science (Honours)
Computer Science
Minor in Labour Studies
Musik is a local music library app for iOS with easy-to-use, always-available controls. Music app designed for those who still download their music library to their devices, while providing easy navigation throughout your library.
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| Top |
Functions
Description
Mathematical and physical constants and constants manipulation functions.
The sources are:
High precision mathematical constants obtained from MPFR.
Fundamental constants: 2018 CODATA recommended values, see constants.txt distributed with NumCosmo sources.
The atomic weights: Commission on Isotopic Abundances and Atomic Weights (CIAAW) of the International Union of Pure and Applied Chemistry (IUPAC). See also from the NIST compilation.
Astronomical constants: IAU 2015 resolutions for the astronomical unit
ncm_c_au()
, parsecncm_c_pc()
and derived constants. See also Luzum 2011.Atomic Spectra: National Institute of Standards and Technology (NIST) Atomic Spectra Standard Reference Database 78 - Version 5.7 (October 2018).
Functions
ncm_c_deg2_steradian ()
long double
ncm_c_deg2_steradian (void
);
The convertion factor from degrees squared to steradian.
ncm_c_stefan_boltzmann ()
gdouble
ncm_c_stefan_boltzmann (void
);
Using CODATA values, see description.
ncm_c_mass_ratio_alpha_p ()
gdouble
ncm_c_mass_ratio_alpha_p (void
);
Using CODATA values, see description.
ncm_c_lightyear ()
gdouble
ncm_c_lightyear (void
);
One year times the speed of light ncm_c_c()
in meters.
ncm_c_fine_struct_square ()
gdouble
ncm_c_fine_struct_square (void
);
Derived from CODATA values, see description.
ncm_c_planck_length2 ()
gdouble
ncm_c_planck_length2 (void
);
Derived from CODATA values, see description.
ncm_c_rest_energy_atomic ()
gdouble
ncm_c_rest_energy_atomic (void
);
Derived from CODATA values, see description.
ncm_c_rest_energy_e ()
gdouble
ncm_c_rest_energy_e (void
);
Derived from CODATA values, see description.
ncm_c_rest_energy_p ()
gdouble
ncm_c_rest_energy_p (void
);
Derived from CODATA values, see description.
ncm_c_rest_energy_n ()
gdouble
ncm_c_rest_energy_n (void
);
Derived from CODATA values, see description.
ncm_c_thermal_wl_e ()
gdouble
ncm_c_thermal_wl_e (void
);
Derived from CODATA values, see description.
The electron termal wavelength is $\lambda_\mathrm{e} = \sqrt{2\pi\hbar^2/(m_\mathrm{e}k_\mathrm{B}T)} \,\left[\mathrm{m}\right]$.
ncm_c_thermal_wl_p ()
gdouble
ncm_c_thermal_wl_p (void
);
Derived from CODATA values, see description.
The proton termal wavelength is $\lambda_\mathrm{p} = \sqrt{2\pi\hbar^2/(m_\mathrm{p}k_\mathrm{B}T)} \,\left[\mathrm{m}\right]$.
ncm_c_thermal_wl_n ()
gdouble
ncm_c_thermal_wl_n (void
);
Derived from CODATA values, see description.
The neutron termal wavelength is $\lambda_\mathrm{n} = \sqrt{2\pi\hbar^2/(m_\mathrm{n}k_\mathrm{B}T)} \,\left[\mathrm{m}\right]$.
ncm_c_thermal_wn_e ()
gdouble
ncm_c_thermal_wn_e (void
);
Derived from CODATA values, see description.
The electron termal wavenumber is $k_\mathrm{e} = 1/\lambda_\mathrm{e}$,
see ncm_c_thermal_wl_e()
.
ncm_c_thermal_wn_p ()
gdouble
ncm_c_thermal_wn_p (void
);
Derived from CODATA values, see description.
The proton termal wavenumber is $k_\mathrm{p} = 1/\lambda_\mathrm{p}$,
see ncm_c_thermal_wl_p()
.
ncm_c_thermal_wn_n ()
gdouble
ncm_c_thermal_wn_n (void
);
Derived from CODATA values, see description.
The neutron termal wavenumber is $k_\mathrm{n} = 1/\lambda_\mathrm{n}$,
see ncm_c_thermal_wl_n()
.
ncm_c_H_reduced_mass ()
gdouble
ncm_c_H_reduced_mass (void
);
Derived from CODATA values, see description.
Reduced mass for the electron in Hydrogen binding energy calculation, i.e., $m_\mathrm{r} = m_\mathrm{e} / (1 + m_\mathrm{e}/m_\mathrm{p})$
ncm_c_H_reduced_energy ()
gdouble
ncm_c_H_reduced_energy (void
);
Reduced mass times $c^2$, $m_\mathrm{r}c^2$, see ncm_c_H_reduced_mass()
.
ncm_c_H_bind ()
gdouble ncm_c_H_bind (const gdouble n
,const gdouble j
);
Energy difference from unbounded state to state $(n,\,j)$, i.e., minus the binding energy of the state $(n,\,j)$, calculated from \begin{equation} E^\mathrm{H}_{n,j} = m_\mathrm{e}c^2\left[1 - f(n,j)\right], \end{equation} where \begin{align} f(n, j) &= \left[1+\left(\frac{\alpha}{n - \delta(j)}\right)^2\right]^{-\frac{1}{2}}, \\ \delta(j) &= j+\frac{1}{2} + \sqrt{\left(j+1/2\right)^2 - \alpha^2}. \end{align}
ncm_c_mass_1H_u ()
gdouble
ncm_c_mass_1H_u (void
);
Obtained from CIAAW commission of IUPAC, see description.
ncm_c_mass_2H_u ()
gdouble
ncm_c_mass_2H_u (void
);
Obtained from CIAAW commission of IUPAC, see description.
ncm_c_mass_3H_u ()
gdouble
ncm_c_mass_3H_u (void
);
Obtained from CIAAW commission of IUPAC, see description.
ncm_c_mass_3He_u ()
gdouble
ncm_c_mass_3He_u (void
);
Obtained from CIAAW commission of IUPAC, see description.
ncm_c_mass_4He_u ()
gdouble
ncm_c_mass_4He_u (void
);
Obtained from CIAAW commission of IUPAC, see description.
ncm_c_mass_1H ()
gdouble
ncm_c_mass_1H (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_1H_u()
$\times$ ncm_c_mass_atomic()
.
ncm_c_mass_2H ()
gdouble
ncm_c_mass_2H (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_2H_u()
$\times$ ncm_c_mass_atomic()
.
ncm_c_mass_3H ()
gdouble
ncm_c_mass_3H (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_3H_u()
$\times$ ncm_c_mass_atomic()
.
ncm_c_mass_3He ()
gdouble
ncm_c_mass_3He (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_3He_u()
$\times$ ncm_c_mass_atomic()
.
ncm_c_mass_4He ()
gdouble
ncm_c_mass_4He (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_4He_u()
$\times$ ncm_c_mass_atomic()
.
ncm_c_rest_energy_1H ()
gdouble
ncm_c_rest_energy_1H (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_1H_u()
$\times$ ncm_c_rest_energy_atomic()
.
ncm_c_rest_energy_2H ()
gdouble
ncm_c_rest_energy_2H (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_2H_u()
$\times$ ncm_c_rest_energy_atomic()
.
ncm_c_rest_energy_3H ()
gdouble
ncm_c_rest_energy_3H (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_3H_u()
$\times$ ncm_c_rest_energy_atomic()
.
ncm_c_rest_energy_3He ()
gdouble
ncm_c_rest_energy_3He (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_3He_u()
$\times$ ncm_c_rest_energy_atomic()
.
ncm_c_rest_energy_4He ()
gdouble
ncm_c_rest_energy_4He (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_4He_u()
$\times$ ncm_c_rest_energy_atomic()
.
ncm_c_mass_ratio_4He_1H ()
gdouble
ncm_c_mass_ratio_4He_1H (void
);
Obtained from CIAAW commission of IUPAC, see description.
Calculated using ncm_c_mass_4He_u()
/ ncm_c_mass_1H_u()
.
ncm_c_au ()
gdouble
ncm_c_au (void
);
Using IAU 2015 recommendation see description, compatible with NASA JPL recommendations (as in 5 January 2016).
ncm_c_G_mass_solar ()
gdouble
ncm_c_G_mass_solar (void
);
Using IAU 2015 recommendation see description.
IAU recomends the use of a fixed value for the gravitational constant times the solar mass.
ncm_c_mass_solar ()
gdouble
ncm_c_mass_solar (void
);
Using IAU 2015 recommendation see description.
As in the recomendation above $\mathrm{M}_\odot = (\mathcal{GM})_\odot / \mathrm{G}$.
Here we use the CODATA 2018 value for $G$, see ncm_c_G()
.
ncm_c_HI_ion_wn_1s_2S0_5 ()
gdouble
ncm_c_HI_ion_wn_1s_2S0_5 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for H-I $1s\,{}^2\!S_{1/2}$ state, i.e., $k_{1s\,{}^2\!S_{1/2}}$.
ncm_c_HI_ion_wn_2s_2S0_5 ()
gdouble
ncm_c_HI_ion_wn_2s_2S0_5 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for H-I $2s\,{}^2\!S_{1/2}$ state calculated
from the difference between the first state and the corresponding Lyman
wavenumber, i.e., $k_{2s\,{}^2\!S_{1/2}} = k_{1s\,{}^2\!S_{1/2}} - k_{2s\,{}^2\!S_{1/2}}^\mathrm{Ly}$,
see ncm_c_HI_Lyman_wn_2s_2S0_5()
.
ncm_c_HI_ion_wn_2p_2P0_5 ()
gdouble
ncm_c_HI_ion_wn_2p_2P0_5 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for H-I $2p\,{}^2\!P_{1/2}$ state calculated
from the difference between the first state and the corresponding Lyman
wavenumber, i.e., $k_{2p\,{}^2\!P_{1/2}} = k_{1s\,{}^2\!S_{1/2}} - k_{2p\,{}^2\!P_{1/2}}^\mathrm{Ly}$,
see ncm_c_HI_Lyman_wn_2p_2P0_5()
.
ncm_c_HI_ion_wn_2p_2P3_5 ()
gdouble
ncm_c_HI_ion_wn_2p_2P3_5 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for H-I $2p\,{}^2\!P_{3/2}$ state calculated
from the difference between the first state and the corresponding Lyman
wavenumber, i.e., $k_{2p\,{}^2\!P_{3/2}} = k_{1s\,{}^2\!S_{3/2}} - k_{2p\,{}^2\!P_{3/2}}^\mathrm{Ly}$,
see ncm_c_HI_Lyman_wn_2p_2P3_5()
.
ncm_c_HI_ion_wn_2p_2Pmean ()
gdouble
ncm_c_HI_ion_wn_2p_2Pmean (void
);
NIST compilation of atomic spectra see description.
The mean ionization energy wavenumber for H-I $2p\,{}^2\!P_{1/2}$ and
$2p\,{}^2\!P_{3/2}$ states , i.e., $k_{2p\,{}^2\!P_\mathrm{mean}} = (k_{2p\,{}^2\!P_{1/2}} + k_{2p\,{}^2\!P_{3/2}}) / 2$,
see ncm_c_HI_Lyman_wn_2p_2Pmean()
.
ncm_c_HI_ion_E_1s_2S0_5 ()
gdouble
ncm_c_HI_ion_E_1s_2S0_5 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{1s\,{}^2\!S_{1/2}}$,
see ncm_c_HI_ion_wn_1s_2S0_5()
.
ncm_c_HI_ion_E_2s_2S0_5 ()
gdouble
ncm_c_HI_ion_E_2s_2S0_5 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2s\,{}^2\!S_{1/2}}$,
see ncm_c_HI_ion_wn_2s_2S0_5()
.
ncm_c_HI_ion_E_2p_2P0_5 ()
gdouble
ncm_c_HI_ion_E_2p_2P0_5 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2p\,{}^2\!P_{1/2}}$,
see ncm_c_HI_ion_wn_2p_2P0_5()
.
ncm_c_HI_ion_E_2p_2P3_5 ()
gdouble
ncm_c_HI_ion_E_2p_2P3_5 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2p\,{}^2\!P_{3/2}}$,
see ncm_c_HI_ion_wn_2p_2P3_5()
.
ncm_c_HI_ion_E_2p_2Pmean ()
gdouble
ncm_c_HI_ion_E_2p_2Pmean (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2p\,{}^2\!P_\mathrm{mean}}$,
see ncm_c_HI_ion_wn_2p_2Pmean()
.
ncm_c_HI_Lyman_wn_2s_2S0_5 ()
gdouble
ncm_c_HI_Lyman_wn_2s_2S0_5 (void
);
NIST compilation of atomic spectra see description.
Lyman emission wavenumber for the $2s\,{}^2\!S_{1/2} \to 1s\,{}^2\!S_{1/2}$ transition $k_{2s\,{}^2\!S_{1/2}}^\mathrm{Ly}$.
ncm_c_HI_Lyman_wn_2p_2P0_5 ()
gdouble
ncm_c_HI_Lyman_wn_2p_2P0_5 (void
);
NIST compilation of atomic spectra see description.
Lyman emission wavenumber for the $2p\,{}^2\!P_{1/2} \to 1s\,{}^2\!S_{1/2}$ transition $k_{2p\,{}^2\!P_{1/2}}^\mathrm{Ly}$.
ncm_c_HI_Lyman_wn_2p_2P3_5 ()
gdouble
ncm_c_HI_Lyman_wn_2p_2P3_5 (void
);
NIST compilation of atomic spectra see description.
Lyman emission wavenumber for the $2p\,{}^2\!P_{3/2} \to 1s\,{}^2\!S_{1/2}$ transition $k_{2p\,{}^2\!P_{3/2}}^\mathrm{Ly}$.
ncm_c_HI_Lyman_wn_2p_2Pmean ()
gdouble
ncm_c_HI_Lyman_wn_2p_2Pmean (void
);
NIST compilation of atomic spectra see description.
Mean Lyman emission wavenumber for the $2p\,{}^2\!P_{1/2}$ and $2p\,{}^2\!P_{3/2}$ states, $k_{2p\,{}^2\!P_{mean}^\mathrm{Ly}} = (k_{2p\,{}^2\!P_{1/2}}^\mathrm{Ly} + k_{2p\,{}^2\!P_{3/2}}^\mathrm{Ly}) / 2$.
ncm_c_HI_Lyman_wl_2s_2S0_5 ()
gdouble
ncm_c_HI_Lyman_wl_2s_2S0_5 (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2s\,{}^2\!S_{1/2} \to 1s\,{}^2\!S_{1/2}$ transition
$\lambda_{2s\,{}^2\!S_{1/2}}^\mathrm{Ly} = \left(k_{2s\,{}^2\!S_{1/2}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HI_Lyman_wn_2s_2S0_5()
.
ncm_c_HI_Lyman_wl_2p_2P0_5 ()
gdouble
ncm_c_HI_Lyman_wl_2p_2P0_5 (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2p\,{}^2\!P_{1/2} \to 1s\,{}^2\!S_{1/2}$ transition
$\lambda_{2p\,{}^2\!P_{1/2}}^\mathrm{Ly} = \left(k_{2p\,{}^2\!P_{1/2}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HI_Lyman_wn_2p_2P0_5()
.
ncm_c_HI_Lyman_wl_2p_2P3_5 ()
gdouble
ncm_c_HI_Lyman_wl_2p_2P3_5 (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2p\,{}^2\!P_{3/2} \to 1s\,{}^2\!S_{1/2}$ transition
$\lambda_{2p\,{}^2\!P_{3/2}}^\mathrm{Ly} = \left(k_{2p\,{}^2\!P_{3/2}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HI_Lyman_wn_2p_2P3_5()
.
ncm_c_HI_Lyman_wl_2p_2Pmean ()
gdouble
ncm_c_HI_Lyman_wl_2p_2Pmean (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2p\,{}^2\!P_\mathrm{mean} \to 1s\,{}^2\!S_{1/2}$ transition
$\lambda_{2p\,{}^2\!P_\mathrm{mean}}^\mathrm{Ly} = \left(k_{2p\,{}^2\!P_\mathrm{mean}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HI_Lyman_wn_2p_2Pmean()
.
ncm_c_HI_Lyman_wl3_8pi_2s_2S0_5 ()
gdouble
ncm_c_HI_Lyman_wl3_8pi_2s_2S0_5 (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2s\,{}^2\!S_{1/2}} = \left(\lambda_{2s\,{}^2\!S_{1/2}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HI_Lyman_wl_2s_2S0_5()
.
ncm_c_HI_Lyman_wl3_8pi_2p_2P0_5 ()
gdouble
ncm_c_HI_Lyman_wl3_8pi_2p_2P0_5 (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2p\,{}^2\!P_{1/2}} = \left(\lambda_{2p\,{}^2\!P_{1/2}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HI_Lyman_wl_2p_2P0_5()
.
ncm_c_HI_Lyman_wl3_8pi_2p_2P3_5 ()
gdouble
ncm_c_HI_Lyman_wl3_8pi_2p_2P3_5 (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2p\,{}^2\!P_{3/2}} = \left(\lambda_{2p\,{}^2\!P_{3/2}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HI_Lyman_wl_2p_2P3_5()
.
ncm_c_HI_Lyman_wl3_8pi_2p_2Pmean ()
gdouble
ncm_c_HI_Lyman_wl3_8pi_2p_2Pmean (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2p\,{}^2\!P_\mathrm{mean}} = \left(\lambda_{2p\,{}^2\!P_\mathrm{mean}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HI_Lyman_wl_2p_2Pmean()
.
ncm_c_boltzmann_factor_HI_1s_2S0_5 ()
gdouble
ncm_c_boltzmann_factor_HI_1s_2S0_5 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{1s\,{}^2\!S_{1/2}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{1s\,{}^2\!S_{1/2}} / (k_\mathrm{B}T)\right]$,
for the $1s\,{}^2\!S_{1/2}$ hydrogen energy level, see
ncm_c_HI_ion_E_1s_2S0_5()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HI_2s_2S0_5 ()
gdouble
ncm_c_boltzmann_factor_HI_2s_2S0_5 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2s\,{}^2\!S_{1/2}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2s\,{}^2\!S_{1/2}} / (k_\mathrm{B}T)\right]$,
for the $2s\,{}^2\!S_{1/2}$ hydrogen energy level, see
ncm_c_HI_ion_E_2s_2S0_5()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HI_2p_2P0_5 ()
gdouble
ncm_c_boltzmann_factor_HI_2p_2P0_5 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2p\,{}^2\!P_{1/2}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2p\,{}^2\!P_{1/2}} / (k_\mathrm{B}T)\right]$,
for the $2p\,{}^2\!P_{1/2}$ hydrogen energy level, see
ncm_c_HI_ion_E_2p_2P0_5()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HI_2p_2P3_5 ()
gdouble
ncm_c_boltzmann_factor_HI_2p_2P3_5 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2p\,{}^2\!P_{3/2}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2p\,{}^2\!P_{3/2}} / (k_\mathrm{B}T)\right]$,
for the $2p\,{}^2\!P_{3/2}$ hydrogen energy level, see
ncm_c_HI_ion_E_2p_2P3_5()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HI_2p_2Pmean ()
gdouble
ncm_c_boltzmann_factor_HI_2p_2Pmean (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2p\,{}^2\!P_\mathrm{mean}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2p\,{}^2\!P_\mathrm{mean}} / (k_\mathrm{B}T)\right]$,
for the $2p\,{}^2\!P_\mathrm{mean}$ hydrogen energy level, see
ncm_c_HI_ion_E_2p_2Pmean()
and ncm_c_thermal_wn_e()
.
ncm_c_HeI_ion_wn_1s_1S0 ()
gdouble
ncm_c_HeI_ion_wn_1s_1S0 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for He-I $1s\,{}^1\!S_{0}$ state, i.e., $k_{1s\,{}^1\!S_{0}}$.
ncm_c_HeI_ion_wn_2s_1S0 ()
gdouble
ncm_c_HeI_ion_wn_2s_1S0 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for He-I $2s\,{}^1\!S_{0}$ state calculated
from the difference between the first state and the corresponding Lyman
wavenumber, i.e., $k_{2s\,{}^1\!S_{0}} = k_{1s\,{}^1\!S_{0}} - k_{2s\,{}^1\!S_{0}}^\mathrm{Ly}$,
see ncm_c_HeI_Lyman_wn_2s_1S0()
.
ncm_c_HeI_ion_wn_2s_3S1 ()
gdouble
ncm_c_HeI_ion_wn_2s_3S1 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for He-I $2s\,{}^3\!S_{1}$ state calculated
from the difference between the first state and the corresponding Lyman
wavenumber, i.e., $k_{2s\,{}^3\!S_{1}} = k_{1s\,{}^1\!S_{0}} - k_{2s\,{}^3\!S_{1}}^\mathrm{Ly}$,
see ncm_c_HeI_Lyman_wn_2s_3S1()
.
ncm_c_HeI_ion_wn_2p_1P1 ()
gdouble
ncm_c_HeI_ion_wn_2p_1P1 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for He-I $2p\,{}^1\!P_{1}$ state calculated
from the difference between the first state and the corresponding Lyman
wavenumber, i.e., $k_{2p\,{}^1\!P_{1}} = k_{1s\,{}^1\!S_{0}} - k_{2p\,{}^1\!P_{1}}^\mathrm{Ly}$,
see ncm_c_HeI_Lyman_wn_2p_1P1()
.
ncm_c_HeI_ion_wn_2p_3P0 ()
gdouble
ncm_c_HeI_ion_wn_2p_3P0 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for He-I $2p\,{}^3\!P_{0}$ state calculated
from the difference between the first state and the corresponding Lyman
wavenumber, i.e., $k_{2p\,{}^3\!P_{0}} = k_{1s\,{}^1\!S_{0}} - k_{2p\,{}^3\!P_{0}}^\mathrm{Ly}$,
see ncm_c_HeI_Lyman_wn_2p_3P0()
.
ncm_c_HeI_ion_wn_2p_3P1 ()
gdouble
ncm_c_HeI_ion_wn_2p_3P1 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for He-I $2p\,{}^3\!P_{1}$ state calculated
from the difference between the first state and the corresponding Lyman
wavenumber, i.e., $k_{2p\,{}^3\!P_{1}} = k_{1s\,{}^1\!S_{0}} - k_{2p\,{}^3\!P_{1}}^\mathrm{Ly}$,
see ncm_c_HeI_Lyman_wn_2p_3P1()
.
ncm_c_HeI_ion_wn_2p_3P2 ()
gdouble
ncm_c_HeI_ion_wn_2p_3P2 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for He-I $2p\,{}^3\!P_{2}$ state calculated
from the difference between the first state and the corresponding Lyman
wavenumber, i.e., $k_{2p\,{}^3\!P_{2}} = k_{1s\,{}^1\!S_{0}} - k_{2p\,{}^3\!P_{2}}^\mathrm{Ly}$,
see ncm_c_HeI_Lyman_wn_2p_3P2()
.
ncm_c_HeI_ion_wn_2p_3Pmean ()
gdouble
ncm_c_HeI_ion_wn_2p_3Pmean (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for He-I $2p\,{}^3\!P_\mathrm{mean}$ state calculated
from the difference between the first state and the corresponding Lyman
wavenumber, i.e., $k_{2p\,{}^3\!P_{0}} = k_{1s\,{}^1\!S_{0}} - k_{2p\,{}^3\!P_\mathrm{mean}}^\mathrm{Ly}$,
see ncm_c_HeI_Lyman_wn_2p_3Pmean()
.
ncm_c_HeI_ion_E_1s_1S0 ()
gdouble
ncm_c_HeI_ion_E_1s_1S0 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{1s\,{}^1\!S_{0}}$,
see ncm_c_HeI_ion_wn_1s_1S0()
.
ncm_c_HeI_ion_E_2s_1S0 ()
gdouble
ncm_c_HeI_ion_E_2s_1S0 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2s\,{}^1\!S_{0}}$,
see ncm_c_HeI_ion_wn_2s_1S0()
.
ncm_c_HeI_ion_E_2s_3S1 ()
gdouble
ncm_c_HeI_ion_E_2s_3S1 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2s\,{}^3\!S_{1}}$,
see ncm_c_HeI_ion_wn_2s_3S1()
.
ncm_c_HeI_ion_E_2p_1P1 ()
gdouble
ncm_c_HeI_ion_E_2p_1P1 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2p\,{}^1\!P_{1}}$,
see ncm_c_HeI_ion_wn_2p_1P1()
.
ncm_c_HeI_ion_E_2p_3P0 ()
gdouble
ncm_c_HeI_ion_E_2p_3P0 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2p\,{}^3\!P_{0}}$,
see ncm_c_HeI_ion_wn_2p_3P0()
.
ncm_c_HeI_ion_E_2p_3P1 ()
gdouble
ncm_c_HeI_ion_E_2p_3P1 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2p\,{}^3\!P_{1}}$,
see ncm_c_HeI_ion_wn_2p_3P1()
.
ncm_c_HeI_ion_E_2p_3P2 ()
gdouble
ncm_c_HeI_ion_E_2p_3P2 (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2p\,{}^3\!P_{2}}$,
see ncm_c_HeI_ion_wn_2p_3P2()
.
ncm_c_HeI_ion_E_2p_3Pmean ()
gdouble
ncm_c_HeI_ion_E_2p_3Pmean (void
);
NIST compilation of atomic spectra see description.
Ionization energy calculated from the wavenumber $k_{2p\,{}^3\!P_\mathrm{mean}}$,
see ncm_c_HeI_ion_wn_2p_3Pmean()
.
ncm_c_HeI_Lyman_wn_2s_1S0 ()
gdouble
ncm_c_HeI_Lyman_wn_2s_1S0 (void
);
NIST compilation of atomic spectra see description.
Lyman emission wavenumber for the $2s\,{}^1\!S_{0} \to 1s\,{}^1\!S_{0}$ transition $k_{2s\,{}^1\!S_{0}}^\mathrm{Ly}$.
ncm_c_HeI_Lyman_wn_2s_3S1 ()
gdouble
ncm_c_HeI_Lyman_wn_2s_3S1 (void
);
NIST compilation of atomic spectra see description.
Lyman emission wavenumber for the $2s\,{}^3\!S_{1} \to 1s\,{}^1\!S_{0}$ transition $k_{2s\,{}^3\!S_{1}}^\mathrm{Ly}$.
ncm_c_HeI_Lyman_wn_2p_1P1 ()
gdouble
ncm_c_HeI_Lyman_wn_2p_1P1 (void
);
NIST compilation of atomic spectra see description.
Lyman emission wavenumber for the $2p\,{}^1\!P_{1} \to 1s\,{}^1\!S_{0}$ transition $k_{2p\,{}^1\!P_{1}}^\mathrm{Ly}$.
ncm_c_HeI_Lyman_wn_2p_3P0 ()
gdouble
ncm_c_HeI_Lyman_wn_2p_3P0 (void
);
NIST compilation of atomic spectra see description.
Lyman emission wavenumber for the $2p\,{}^3\!P_{0} \to 1s\,{}^1\!S_{0}$ transition $k_{2p\,{}^3\!P_{0}}^\mathrm{Ly}$.
ncm_c_HeI_Lyman_wn_2p_3P1 ()
gdouble
ncm_c_HeI_Lyman_wn_2p_3P1 (void
);
NIST compilation of atomic spectra see description.
Lyman emission wavenumber for the $2p\,{}^3\!P_{1} \to 1s\,{}^1\!S_{0}$ transition $k_{2p\,{}^3\!P_{1}}^\mathrm{Ly}$.
ncm_c_HeI_Lyman_wn_2p_3P2 ()
gdouble
ncm_c_HeI_Lyman_wn_2p_3P2 (void
);
NIST compilation of atomic spectra see description.
Lyman emission wavenumber for the $2p\,{}^3\!P_{2} \to 1s\,{}^1\!S_{0}$ transition $k_{2p\,{}^3\!P_{2}}^\mathrm{Ly}$.
ncm_c_HeI_Lyman_wn_2p_3Pmean ()
gdouble
ncm_c_HeI_Lyman_wn_2p_3Pmean (void
);
NIST compilation of atomic spectra see description.
Mean Lyman emission wavenumber for the $2p\,{}^3\!P_{*}$, i.e.,
$k_{2p\,{}^3\!P_\mathrm{mean}}^\mathrm{Ly} = \left(k_{2p\,{}^3\!P_{0}}^\mathrm{Ly} + k_{2p\,{}^3\!P_{1}}^\mathrm{Ly} + k_{2p\,{}^3\!P_{2}}^\mathrm{Ly}\right) / 3$.
See ncm_c_HeI_Lyman_wn_2p_3P0()
, ncm_c_HeI_Lyman_wn_2p_3P1()
and ncm_c_HeI_Lyman_wn_2p_3P2()
.
ncm_c_HeI_Lyman_wl_2s_1S0 ()
gdouble
ncm_c_HeI_Lyman_wl_2s_1S0 (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2s\,{}^1\!S_{0} \to 1s\,{}^1\!S_{0}$ transition
$\lambda_{2s\,{}^1\!S_{0}}^\mathrm{Ly} = \left(k_{2s\,{}^1\!S_{0}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HeI_Lyman_wn_2s_1S0()
.
ncm_c_HeI_Lyman_wl_2s_3S1 ()
gdouble
ncm_c_HeI_Lyman_wl_2s_3S1 (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2s\,{}^3\!S_{1} \to 1s\,{}^1\!S_{0}$ transition
$\lambda_{2s\,{}^3\!S_{1}}^\mathrm{Ly} = \left(k_{2s\,{}^3\!S_{1}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HeI_Lyman_wn_2s_3S1()
.
ncm_c_HeI_Lyman_wl_2p_1P1 ()
gdouble
ncm_c_HeI_Lyman_wl_2p_1P1 (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2p\,{}^1\!P_{1} \to 1s\,{}^1\!S_{0}$ transition
$\lambda_{2p\,{}^1\!P_{1}}^\mathrm{Ly} = \left(k_{2p\,{}^1\!P_{1}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HeI_Lyman_wn_2p_1P1()
.
ncm_c_HeI_Lyman_wl_2p_3P0 ()
gdouble
ncm_c_HeI_Lyman_wl_2p_3P0 (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2p\,{}^3\!P_{0} \to 1s\,{}^1\!S_{0}$ transition
$\lambda_{2p\,{}^3\!P_{0}}^\mathrm{Ly} = \left(k_{2p\,{}^3\!P_{0}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HeI_Lyman_wn_2p_3P0()
.
ncm_c_HeI_Lyman_wl_2p_3P1 ()
gdouble
ncm_c_HeI_Lyman_wl_2p_3P1 (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2p\,{}^3\!P_{1} \to 1s\,{}^1\!S_{0}$ transition
$\lambda_{2p\,{}^3\!P_{1}}^\mathrm{Ly} = \left(k_{2p\,{}^3\!P_{1}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HeI_Lyman_wn_2p_3P1()
.
ncm_c_HeI_Lyman_wl_2p_3P2 ()
gdouble
ncm_c_HeI_Lyman_wl_2p_3P2 (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2p\,{}^3\!P_{2} \to 1s\,{}^1\!S_{0}$ transition
$\lambda_{2p\,{}^3\!P_{2}}^\mathrm{Ly} = \left(k_{2p\,{}^3\!P_{2}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HeI_Lyman_wn_2p_3P2()
.
ncm_c_HeI_Lyman_wl_2p_3Pmean ()
gdouble
ncm_c_HeI_Lyman_wl_2p_3Pmean (void
);
NIST compilation of atomic spectra see description.
Wavelength for the $2p\,{}^3\!P_\mathrm{mean} \to 1s\,{}^1\!S_{0}$ transition
$\lambda_{2p\,{}^3\!P_\mathrm{mean}}^\mathrm{Ly} = \left(k_{2p\,{}^3\!P_\mathrm{mean}}^\mathrm{Ly}\right)^{-1}$,
see ncm_c_HeI_Lyman_wn_2p_3Pmean()
.
ncm_c_HeI_Lyman_wl3_8pi_2s_1S0 ()
gdouble
ncm_c_HeI_Lyman_wl3_8pi_2s_1S0 (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2s\,{}^1\!S_{0}} = \left(\lambda_{2s\,{}^1\!S_{0}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HeI_Lyman_wl_2s_1S0()
.
ncm_c_HeI_Lyman_wl3_8pi_2s_3S1 ()
gdouble
ncm_c_HeI_Lyman_wl3_8pi_2s_3S1 (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2s\,{}^3\!S_{1}} = \left(\lambda_{2s\,{}^3\!S_{1}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HeI_Lyman_wl_2s_3S1()
.
ncm_c_HeI_Lyman_wl3_8pi_2p_1P1 ()
gdouble
ncm_c_HeI_Lyman_wl3_8pi_2p_1P1 (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2p\,{}^1\!P_{1}} = \left(\lambda_{2p\,{}^1\!P_{1}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HeI_Lyman_wl_2p_1P1()
.
ncm_c_HeI_Lyman_wl3_8pi_2p_3P0 ()
gdouble
ncm_c_HeI_Lyman_wl3_8pi_2p_3P0 (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2p\,{}^3\!P_{0}} = \left(\lambda_{2p\,{}^3\!P_{0}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HeI_Lyman_wl_2p_3P0()
.
ncm_c_HeI_Lyman_wl3_8pi_2p_3P1 ()
gdouble
ncm_c_HeI_Lyman_wl3_8pi_2p_3P1 (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2p\,{}^3\!P_{1}} = \left(\lambda_{2p\,{}^3\!P_{1}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HeI_Lyman_wl_2p_3P1()
.
ncm_c_HeI_Lyman_wl3_8pi_2p_3P2 ()
gdouble
ncm_c_HeI_Lyman_wl3_8pi_2p_3P2 (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2p\,{}^3\!P_{2}} = \left(\lambda_{2p\,{}^3\!P_{2}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HeI_Lyman_wl_2p_3P2()
.
ncm_c_HeI_Lyman_wl3_8pi_2p_3Pmean ()
gdouble
ncm_c_HeI_Lyman_wl3_8pi_2p_3Pmean (void
);
NIST compilation of atomic spectra see description.
Effective volume of the Lyman wavelength $V^\mathrm{Ly}_{2p\,{}^3\!P_\mathrm{mean}} = \left(\lambda_{2p\,{}^3\!P_\mathrm{mean}}^\mathrm{Ly}\right)^{3} / (8\pi)$,
see ncm_c_HeI_Lyman_wl_2p_3Pmean()
.
ncm_c_boltzmann_factor_HeI_1s_1S0 ()
gdouble
ncm_c_boltzmann_factor_HeI_1s_1S0 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{1s\,{}^1\!S_{0}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{1s\,{}^1\!S_{0}} / (k_\mathrm{B}T)\right]$,
for the $1s\,{}^1\!S_{0}$ helium energy level, see
ncm_c_HeI_ion_E_1s_1S0()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HeI_2s_1S0 ()
gdouble
ncm_c_boltzmann_factor_HeI_2s_1S0 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2s\,{}^1\!S_{0}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2s\,{}^1\!S_{0}} / (k_\mathrm{B}T)\right]$,
for the $2s\,{}^1\!S_{0}$ helium energy level, see
ncm_c_HeI_ion_E_2s_1S0()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HeI_2s_3S1 ()
gdouble
ncm_c_boltzmann_factor_HeI_2s_3S1 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2s\,{}^3\!S_{1}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2s\,{}^3\!S_{1}} / (k_\mathrm{B}T)\right]$,
for the $2s\,{}^3\!S_{1}$ helium energy level, see
ncm_c_HeI_ion_E_2s_3S1()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HeI_2p_1P1 ()
gdouble
ncm_c_boltzmann_factor_HeI_2p_1P1 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2p\,{}^1\!P_{1}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2p\,{}^1\!P_{1}} / (k_\mathrm{B}T)\right]$,
for the $2p\,{}^1\!P_{1}$ helium energy level, see
ncm_c_HeI_ion_E_2p_1P1()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HeI_2p_3P0 ()
gdouble
ncm_c_boltzmann_factor_HeI_2p_3P0 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2p\,{}^3\!P_{0}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2p\,{}^3\!P_{0}} / (k_\mathrm{B}T)\right]$,
for the $2p\,{}^3\!P_{0}$ helium energy level, see
ncm_c_HeI_ion_E_2p_3P0()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HeI_2p_3P1 ()
gdouble
ncm_c_boltzmann_factor_HeI_2p_3P1 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2p\,{}^3\!P_{1}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2p\,{}^3\!P_{1}} / (k_\mathrm{B}T)\right]$,
for the $2p\,{}^3\!P_{1}$ helium energy level, see
ncm_c_HeI_ion_E_2p_3P1()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HeI_2p_3P2 ()
gdouble
ncm_c_boltzmann_factor_HeI_2p_3P2 (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2p\,{}^3\!P_{2}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2p\,{}^3\!P_{2}} / (k_\mathrm{B}T)\right]$,
for the $2p\,{}^3\!P_{2}$ helium energy level, see
ncm_c_HeI_ion_E_2p_3P2()
and ncm_c_thermal_wn_e()
.
ncm_c_boltzmann_factor_HeI_2p_3Pmean ()
gdouble
ncm_c_boltzmann_factor_HeI_2p_3Pmean (const gdouble T
);
NIST compilation of atomic spectra see description.
Calculates the Boltzmann factor $B_{2p\,{}^3\!P_\mathrm{mean}}(T) = k_\mathrm{e}^3 T^{-3/2}\,\exp\left[-E_{2p\,{}^3\!P_\mathrm{mean}} / (k_\mathrm{B}T)\right]$,
for the $2p\,{}^3\!P_\mathrm{mean}$ helium energy level, see
ncm_c_HeI_ion_E_2p_3Pmean()
and ncm_c_thermal_wn_e()
.
ncm_c_HeI_Balmer_wn_2p_1P1_2s_1S0 ()
gdouble
ncm_c_HeI_Balmer_wn_2p_1P1_2s_1S0 (void
);
NIST compilation of atomic spectra see description.
Balmer emission wavenumber for the $2p\,{}^1\!P_{1} \to 2s\,{}^1\!S_{0}$ transition $k_{2p\,{}^1\!P_{1}}^{2s\,{}^1\!S_{0}}$, calculated from the difference between the Lyman lines $2s\,{}^1\!S_{0}$ state and the corresponding Lyman wavenumber, i.e., $k_{2p\,{}^1\!P_{1}}^{2s\,{}^1\!S_{0}} = k_{2p\,{}^1\!P_{1}}^\mathrm{Ly} - k_{2s\,{}^1\!S_{0}}^\mathrm{Ly}$.
ncm_c_HeI_Balmer_wn_2p_3Pmean_2s_3S1 ()
gdouble
ncm_c_HeI_Balmer_wn_2p_3Pmean_2s_3S1 (void
);
NIST compilation of atomic spectra see description.
Balmer emission wavenumber for the $2p\,{}^3\!P_\mathrm{mean} \to 2s\,{}^3\!S_{1}$ transition $k_{2p\,{}^3\!P_\mathrm{mean}}^{2s\,{}^3\!S_{1}}$, calculated from the difference between the Lyman lines $2s\,{}^1\!S_{0}$ state and the corresponding Lyman wavenumber, i.e., $k_{2p\,{}^3\!P_\mathrm{mean}}^{2s\,{}^3\!S_{1}} = k_{2p\,{}^3\!P_\mathrm{mean}}^\mathrm{Ly} - k_{2s\,{}^3\!S_{1}}^\mathrm{Ly}$.
ncm_c_HeI_Balmer_E_kb_2p_1P1_2s_1S0 ()
gdouble
ncm_c_HeI_Balmer_E_kb_2p_1P1_2s_1S0 (void
);
NIST compilation of atomic spectra see description.
Balmer emission energy $E_{2p\,{}^1\!P_{1}}^{2s\,{}^1\!S_{0}} = hc\times{}k_{2p\,{}^1\!P_{1}}^{2s\,{}^1\!S_{0}}$ over $k_\mathrm{B}$.
ncm_c_HeI_Balmer_E_kb_2p_3Pmean_2s_3S1 ()
gdouble
ncm_c_HeI_Balmer_E_kb_2p_3Pmean_2s_3S1
(void
);
NIST compilation of atomic spectra see description.
Balmer emission energy $E_{2p\,{}^3\!P_\mathrm{mean}}^{2s\,{}^3\!S_{1}} = hc\times{}k_{2p\,{}^3\!P_\mathrm{mean}}^{2s\,{}^3\!S_{1}}$ over $k_\mathrm{B}$.
ncm_c_HeII_ion_wn_1s_2S0_5 ()
gdouble
ncm_c_HeII_ion_wn_1s_2S0_5 (void
);
NIST compilation of atomic spectra see description.
Ionization energy wavenumber for He-II $1s\,{}^2\!S_{1/2}$ state, i.e., $k_{1s\,{}^2\!S_{1/2}}$.
ncm_c_HeII_ion_E_1s_2S0_5 ()
gdouble
ncm_c_HeII_ion_E_1s_2S0_5 (void
);
Ionization energy for He-II $1s\,{}^2\!S_{1/2}$ state, i.e., $E_{1s\,{}^2\!S_{1/2}} = hc \times k_{1s\,{}^2\!S_{1/2}}$.
ncm_c_decay_H_rate_2s_1s ()
gdouble
ncm_c_decay_H_rate_2s_1s (void
);
Theoretical value for the two photons decay rate for Hydrogen $2\mathrm{s} \to 1\mathrm{s}$ states Goldman 1989.
ncm_c_decay_He_rate_2s_1s ()
gdouble
ncm_c_decay_He_rate_2s_1s (void
);
Theoretical value for the two photons decay rate for Helium $2\mathrm{s} \to 1\mathrm{s}$ states Drake 1969.
ncm_c_stats_1sigma ()
long double
ncm_c_stats_1sigma (void
);
The integral of a Gaussian distribution with mean $\mu$ and standard deviation $\sigma$ in $(\mu - 1 \sigma, \mu + 1 \sigma)$.
ncm_c_stats_2sigma ()
long double
ncm_c_stats_2sigma (void
);
The integral of a Gaussian distribution with mean $\mu$ and standard deviation $\sigma$ in $(\mu - 2 \sigma, \mu + 2 \sigma)$.
ncm_c_stats_3sigma ()
long double
ncm_c_stats_3sigma (void
);
The integral of a Gaussian distribution with mean $\mu$ and standard deviation sigma in $(\mu - 3 \sigma, \mu + 3 \sigma)$.
ncm_c_wmap5_coadded_I_K ()
gdouble
ncm_c_wmap5_coadded_I_K (void
);
WMAP-5 noise per observation for resolution 9 and 10 $I$ maps, to $\sim$0.1% uncertainty for differencing assembly (DA) $\text{K1}$. See Hinshaw (2009) [arXiv].
ncm_c_wmap5_coadded_I_Ka ()
gdouble
ncm_c_wmap5_coadded_I_Ka (void
);
WMAP-5 noise per observation for resolution 9 and 10 $I$ maps, to $\sim$0.1% uncertainty for differencing assembly (DA) $\text{Ka1}$. See Hinshaw (2009) [arXiv].
ncm_c_wmap5_coadded_I_Q ()
gdouble
ncm_c_wmap5_coadded_I_Q (void
);
WMAP-5 noise per observation for resolution 9 and 10 $I$ maps, to $\sim$0.1% uncertainty for differencing assembly (DA) $\text{Q}$. See Smidt (2009) [arXiv].
ncm_c_wmap5_coadded_I_V ()
gdouble
ncm_c_wmap5_coadded_I_V (void
);
WMAP-5 noise per observation for resolution 9 and 10 $I$ maps, to $\sim$0.1% uncertainty for differencing assembly (DA) $\text{V}$. See Smidt (2009) [arXiv].
ncm_c_wmap5_coadded_I_W ()
gdouble
ncm_c_wmap5_coadded_I_W (void
);
WMAP-5 noise per observation for resolution 9 and 10 $I$ maps, to $\sim$0.1% uncertainty for differencing assembly (DA) $\text{W}$. See Smidt (2009) [arXiv].
ncm_c_hubble_cte_planck6_base ()
gdouble
ncm_c_hubble_cte_planck6_base (void
);
Planck VI Hubble constant base-$\Lambda$CDM model TT,TE,EE$+$lowE$+$lensing final result. See Planck Collaboration (2018) [arXiv].
ncm_c_hubble_cte_hst ()
gdouble
ncm_c_hubble_cte_hst (void
);
HST Hubble constant final result. See Freedman (2001) [arXiv].
ncm_c_hubble_radius_hm1_Mpc ()
gdouble
ncm_c_hubble_radius_hm1_Mpc (void
);
Hubble radius in units of $\mathsf{h}^{-1} \, \text{Mpc}$ defined as
\begin{equation}
R_H h^{-1} = \frac{c}{100 \mathsf{h} \, \text{km} \, \text{sec}^{-1} \, \text{Mpc}^{-1}} \, ,
\end{equation}
where $c$ is the speed of light (ncm_c_c()
). Calculated using ncm_c_c()
$/$ $10^{5}$.
ncm_c_hubble_radius_hm1_planck ()
gdouble
ncm_c_hubble_radius_hm1_planck (void
);
Hubble radius in units of $\mathsf{h}^{-1} \, l_{\text{p}}$. Calculated using ncm_c_hubble_radius_hm1_Mpc()
$\times$ ncm_c_Mpc()
$/$ ncm_c_planck_length()
.
ncm_c_crit_density_h2 ()
gdouble
ncm_c_crit_density_h2 (void
);
The critical density is defined as
\begin{equation}
\rho_{\mathrm{crit}0} = \frac{3 c^2 H_0^2}{8\pi G},
\end{equation}
where $G$ is the gravitational constant (ncm_c_G()
), $c$ is the speed of light
(ncm_c_c()
) and $H_0$ is the Hubble parameter,
$$H_0 = 100 \times \mathsf{h} \,\left[\text{km}\,\text{s}^{-1}\,\text{Mpc}^{-1}\right].$$
ncm_c_crit_mass_density_h2 ()
gdouble
ncm_c_crit_mass_density_h2 (void
);
This function computes the critical mass density over $\mathsf{h}^2 \times c^2$.
ncm_c_crit_mass_density_h2_solar_mass_Mpc3 ()
gdouble
ncm_c_crit_mass_density_h2_solar_mass_Mpc3
(void
);
This function computes the critical mass density in units of solar mass $M_\odot$ and Mpc.
ncm_c_crit_number_density_p ()
gdouble
ncm_c_crit_number_density_p (void
);
This function computes the proton number density in units of its rest energy. Calculated using ncm_c_crit_density_h2()
$/$ ncm_c_rest_energy_p()
.
ncm_c_crit_number_density_n ()
gdouble
ncm_c_crit_number_density_n (void
);
This function computes the neutron number density in units of its rest energy. Calculated using ncm_c_crit_density_h2()
$/$ ncm_c_rest_energy_n()
.
ncm_c_blackbody_energy_density ()
gdouble
ncm_c_blackbody_energy_density (void
);
This functions returns the black body energy density divided by $T^4$. Defined as
\begin{equation}
\frac{\rho_{\text{BL}}}{T^4} = \frac{8\pi^2k_{\text{b}}^4}{15 \left( hc \right)^3},
\end{equation}
where $\rho_{\text{BL}}$ is the black body energy density, $T$ is the temperature, $k_{\text{b}}$ is the Boltzmann constant (ncm_c_kb()
), $h$ is the Planck constant (ncm_c_h()
) and $c$ is the speed of light (ncm_c_c()
).
ncm_c_blackbody_per_crit_density_h2 ()
gdouble
ncm_c_blackbody_per_crit_density_h2 (void
);
This functions returns ncm_c_blackbody_energy_density()
$/$ ncm_c_crit_density_h2()
.


EBD - Easton Bible DIctionary
Salcah
SALCAH
"SALCAH "wandering, a city of Bashan assigned to the half tribe of Manasseh (
Deuteronomy 3:10
;
Joshua 12:5
;
13:11
), identified with Salkhad, about 56 miles east of Jordan.
"SALCAH "wandering, a city of Bashan assigned to the half tribe of Manasseh (Deuteronomy 3:10; Joshua 12:5; 13:11), identified with Salkhad, about 56 miles east of Jordan.


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Before developing the theory, it must be pointed out that the meaning of time becomes complicated in that there are two time variations involved. There is the time associated with the forcing function and this is denoted by the symbol $\tau$. There is also the time associated with the displacement and this is denoted by the symbol t. To all intents and purposes t, the displacement time, can be considered as a constant since it is possible to specify that the response is required at a specific time, at 5 seconds say. The time associated with the force, $\tau$, is the variable since this can take any value between 0 and t.
If the response of the system to a single impulse Rd$\tau$ can be found then the response to all of the impulses and hence the response to the time varying load can be found by summation. To simplify this further consider the impulse Rd$\tau$ to be applied at time zero.
Further, it was shown in section 2.6.1 that the systems eigenvectors can be used to turn a multi-degree of freedom set of dynamic equations into a series of uncoupled, single degree of freedom set. This means that the solution process only has to be developed for a single degree of freedom system, typically
\begin{equation}
m\ddot{r}(t)+c\dot{r}(t)+kr(t) =R(t)
\end{equation}
This can be written in non-dimensional form as
\begin{equation}
\ddot{r}(t)+2\omega_{u}\xi\dot{r}(t)+\omega_{u}^{2}r(t)=\frac{1}{m}R(t)
\end{equation}
Consider an impulse Rd$\tau$ is applied at time zero.
Calling the time just before the impulse is applied $\tau$=-0, then up to this time the system is at rest and both the displacement and the velocity are zero. The impulse causes a change in momentum so that there is an instantaneous change in the velocity at time zero. The impulse does not affect the displacement instantaneously so that at time $\tau$=+0, just after the impulse the initial conditions are
\begin{equation}
r=0 \quad at \quad time \quad \tau=+0 \qquad (149)
\end{equation}
and
\begin{equation}
\dot{r}=\frac{R(\tau)d\tau}{m} \quad at \quad time \quad \tau=+0 \qquad (150)
\end{equation}
It will be seen that the force is zero for $\tau$ $>$ +0 hence the equation of motion (148) becomes
\begin{equation}
\ddot{r}(t)+2\omega_{u}\xi\dot{r}(t)+\omega_{u}^{2}r(t)=0 \quad at \quad time \quad \tau \geq+0
\end{equation}
This has the solution
\begin{equation}
r= r_{01} e^{-\alpha t} sin(\beta t) + r_{02}e^{-\alpha t} cos(\beta t)
\end{equation}
Where
\begin{equation}
\alpha= \omega_{u}\xi
\end{equation}
and
\begin{equation}
\beta = \omega_{u}(1- \xi)^{1/2}
\end{equation}
Using the initial conditions from equations (149) and (150) gives
\begin{equation}
r_{02}=0
\end{equation}
and
\begin{equation}
r_{01} =\frac{1}{\beta m} R(\tau)d\tau
\end{equation}
Hence the response at time t to an impulse applied at $\tau$=0 is
\begin{equation}
r(t)= \frac{1}{\beta m} e^{-\alpha t} sin(\beta t)R(\tau)d\tau \qquad (157)
\end{equation}
If the impulse is applied at some time $\tau$ which is not zero then the response can be found by shifting the origin from 0 to $\tau$. Hence, equation (157) then becomes
\begin{equation}
r(t)= \frac{1}{\beta m} e^{-\alpha (t-\tau)} sin(\beta (t-\tau))R(\tau)d\tau \quad (t \geq \tau)
\end{equation}
Since the problem under consideration is linear then the response at time t to a series of impulses applied at different times $\tau$ is
\begin{equation}
r(t)= \sum_{0}^{t} \frac{1}{\beta m} e^{-\alpha (t-\tau)} sin(\beta (t-\tau))R(\tau)d\tau
\end{equation}
Which, in the limit of d$\tau$ being very small reduces to:
\begin{equation}
r(t) = \int_{0}^{t} \frac{e^{-\alpha (t-\tau)} sin(\beta (t-\tau))}{\beta m} R(\tau)d\tau \qquad (160)
\end{equation}
If at time zero the initial conditions are $r_{0}$ for the displacement and $\dot{r_{0}}$ for the velocity then response becomes
\begin{equation}
r(t) = \int_{0}^{t} \frac{e^{-\alpha (t-\tau)} sin(\beta (t-\tau))}{\beta m} R(\tau)d\tau +r_{0}e^{-\alpha t} cos(\beta t) + \frac{(\dot{r_{0}}+\alpha_{0})e^{-\alpha t}}{\beta}sin(\beta t)
\end{equation}
If the damping is zero then
\begin{equation}
\alpha=0
\end{equation}
and
\begin{equation}
\beta=\omega_{u}
\end{equation}
The response at time t then simplifies to
\begin{equation}
r(t) = \int_{0}^{t} \frac{ sin(\omega_{u} (t-\tau))}{\omega_{u} m} R(\tau)d\tau +r_{0} cos(\omega_{u} t) + \frac{\dot{r_{0}}}{\omega_{u}}{\beta}sin(\omega_{u} t) \qquad (164)
\end{equation}
Equation (164) is known as the convolution integral or the Duhamel integral. It is very often used in the undamped form of equation (164). If both the displacement and the velocity are zero (the structure is at rest at time zero) then the convolution integral can be written in various forms
\begin{equation}
r(t) = \int_{0}^{t} \frac{ sin(\omega_{u} (t-\tau))}{\omega_{u} m} R(\tau)d\tau \qquad (165)
\end{equation}
\begin{equation}
r(t) = \int_{-\infty}^{t} \frac{ sin(\omega_{u} (t-\tau))}{\omega_{u} m} R(\tau)d\tau
\end{equation}
\begin{equation}
r(t) = \int_{0}^{\infty} \frac{ sin(\omega_{u} (t-\tau))}{\omega_{u} m} R(\tau)d\tau \qquad (167)
\end{equation}
\begin{equation}
r(t) = \int_{- \infty}^{\infty} \frac{ sin(\omega_{u} (t-\tau))}{\omega_{u} m} R(\tau)d\tau
\end{equation}
The forms given by equations (165) and (167) are generally the most useful and the form given by (165) will be used here.
The convolution integral in the form of equation (160) is often written as
\begin{equation}
r(t) = \int_{0}^{t} \frac{e^{-\alpha (t-\tau)} sin(\beta (t-\tau))}{\beta m} R(\tau)d\tau
\end{equation}
\begin{equation}
r(t) = \int_{0}^{t} W(t-\tau) R(\tau)d\tau
\end{equation}
Where
\begin{equation}
W(t-\tau)= \frac{e^{-\alpha (t-\tau)} sin(\beta (t-\tau))}{\beta m}
\end{equation}
is called the impulse response function. It represents the response at time t due to an impulse applied at a time $\tau$. This quantity can be measured experimentally.


--- layout: page title: Lean Prover Zulip Chat Archive permalink: archive/113488general/82160inductionintactics.html ---
Say I write a tactic that somewhere uses induction x
for some x
. Now I get back a list of goals. Is it better style to use that list to tackle each goal, or should I use tactic.focus
?


Deprecated API(s) Dashboard
The audit tool output for the following packages were obtained by checking the image and the bundle manifests distributed. This report aims to try to identify the package distributions that can impact the users on 4.9.
Data from the image used
- Image name: registry.redhat.io/redhat/redhat-operator-index:v4.7
- Image ID: sha256:2b5ead228ca899f82b7e9b5165f760a10d7ffde3b97f6ead01cae3ac8c017640
- Image Created at: 2021-09-16T16:50:34.585287912Z
- From JSON report generated at: 2021-09-18
FAQ
1. Can my package still have bundles using deprecated API(s) that are not found by this check?
Yes. The check can only be made by looking at the manifests shipped in the bundle. Your operator might be using the deprecated/removed API(s) but not shipping its manifests on the bundle or have a dependency on another operator that is using them.
2. What action(s) should I take?
- Check Deprecated API Migration Guide (v1.22) and ensure that your projects have been migrated and are not using any deprecated/removed API(s)
- Ensure that any distribution which requires any deprecated API(s) in the OCP catalogs are configured with the Max OpenShift Version compatible (`olm.openShiftMaxVersion`) so it will only be distributed on OCP version(s) <= 4.8. Also, control which version the bundle is deployed to from OLM via the annotation/label `com.redhat.openshift.versions`. More info see: OKD/OpenShift Catalogs criteria and options
- OpenShift 4.8 introduces two new alerts that fire when an API that will be removed in the next release is in use. Check the event alerts of your Operators running on 4.8 and ensure that you do not find any warning about these API(s) still being used by it
3. What does it mean for a package to be in red, amber or green?
- (Green) Complying: these are packages that we cannot found the removed APIs in k8s 1.22/OCP 4.9 in at least one bundle version
- (Amber) Not complying: these are the packages that we cannot found any versions which is not using the removed APIs in in k8s 1.22/OCP 4.9
Using deprecated APIs
| Package Name | Kinds to migrate | Channels | Bundles uses API(s) | Bundles Migrated |
|---|---|---|---|---|
| apicast-operator |
|
|
|
|
Has a bundle that we could not find the deprecate APIs
| Package Name | Kinds to migrate | Channels | Bundles uses API(s) | Bundles Migrated |
|---|


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Not only are the classes broken down into age group, they are also divided into appropriate skill levels. This is so those with similar skill levels may progress and learn adequate to their rank.
Most Classes are divided into the ranks of:
- Beginner Level - White Belt - Green Belt
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1
2
3
4
5
xforms-insert
10.3.i insert action - xforms-insert event
You must have seen an xforms-insert message. The Node Count output must display a value of "6".
Node Count :


The club envisions a society with better knowledge, awareness, and access to technologies around the globe. We believe in achieving solutions of real world problems through using technologies which are either developing, new or old in an innovative way. The key idea is to provide an environment where people can interact, present their ideas, discuss it and modify it for application in our day to day life.
And, it's not always research because we do conduct many National Level Workshops and fun events like Minute-2-Win-it. Our membership drive is free and accessible to journals, internships and many more enthusiastic events.
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Our Project
Our ancestors gave more importance to agriculture and it was basically following all the traditional methods their forefathers followed. As the population increased the need for production was given more importance and the pressure on agriculture increased as the years followed.
5G is the fifth generation network in mobiles. It started with an intention to deliver higher multi–Gbps peak data speeds, ultra low latency, more reliability, large network capacity, increased availability and a uniform userIt began deploying worldwide in 2019. It was successor to the 4G networks which are the connectivity provided for most current mobiles.
If space has always been an enigma for mankind, then the moon has always served as the first post for any attempt at understanding or exploring deeper space. All ventures into outer space, ranging from exploratory fly-bys to managed flights, have first been tried out of the moon .


Python Problems & Solutions For Beginners
Python Problems & Solutions For Beginners
Introduction to python taught through example problems. Solutions are included in embedded repl.it at the bottom of this page for you to practice and refactor.
Python Practice Problems
Here are some other articles for reference if you need them:
Here are the problems without solutions for you to practice with:
Problem 1
Create a program that asks the user to enter their name and
their age. Print out a message addressed to them that tells them
the year that they will turn
100
years old.
The
datetime
module supplies classes for manipulating dates and times.
While date and time arithmetic is supported, the focus of the implementation is on efficient attribute extraction for output formatting and manipulation.
Only one concrete class, the class, is supplied by the module. The class can represent simple timezones with fixed…docs.python.org
Problem 2
Ask the user for a number. Depending on whether the number is
even
or
odd
, print out
an appropriate message to the user.
Bonus:
-
If the number is a multiple of
4
, print out a different message. - Ask the user for two numbers: one number to check (call it num) and one number to divide by (check). If check divides evenly into num, tell that to the user. If not, print a different appropriate message.
Problem 3
Take a list and write a program that prints out all the elements
of the list that are
less
than
5
.
Extras:
-
Instead of printing the elements one by one, make a new list
that has all the elements less than
5
from this list in it and print out this new list. - Write this in one line of Python.
- Ask the user for a number and return a list that contains only elements from the original list a that are smaller than that number given by the user.
Problem 4
Create a program that asks the user for a number and then prints out a list of all the divisors of that number.
For example,
13
is a divisor
of 26
because
26 / 13
has no
remainder.)
Problem 5
Take two lists, and write a program that returns a list that
contains only the elements that are
common between the lists (without duplicates)
. Make sure your program works on two lists of different sizes.
Source code: Lib/random.py This module implements pseudo-random number generators for various distributions. For…docs.python.org
Bonus:
- Randomly generate two lists to test this.
- Write this in one line of Python.
Problem 6
Ask the user for a string and print out whether this string is a
palindrome
or
not. (A palindrome is a string that reads the same forwards and
backwards.)
Here’s 5 ways to reverse a string (courtesy of geeksforgeeks)
Problem 7
Let’s say I give you a list saved in a variable: a =
[1, 4, 9, 16, 25, 36, 49, 64, 81, 100]
.
Write one line of Python that takes this list a and makes a new
list that has only the
even
elements
of this list in it.
Problem 8
Make a two-player
Rock-Paper-Scissors
game.
Hint:
Ask for player plays (using input), compare them. Print
out a message of congratulations to the winner, and ask if the
players want to start a new game.
Problem 9
Generate a random number between
1 and 100 (including 1 and 100)
. Ask the user to guess the number, then tell them whether they
guessed
too low
,
too high
, or
exactly right
.
Hint:
Remember to use the user input from the very first exercise.
Extras:
Keep the game going until the user types
“exit”
.
Keep track of how many guesses the user has taken, and
when the game ends, print this out.
Problem 10
Write a program that asks the user how many Fibonacci numbers to generate and then generates them. Take this opportunity to think about how you can use functions. Make sure to ask the user to enter the number of numbers in the sequence to generate.
Hint:
The Fibonacci sequence is a sequence of numbers where the
next number in the sequence is the sum of the previous two
numbers in the sequence. The sequence looks like this:
1, 1, 2, 3, 5, 8, 13, …
Intermediate Problems:
Problem 11
In linear algebra,
a Toeplitz matrix is one in which the elements on any given
diagonal from top left to bottom right are identical.
Here is an example:
1 2 3 4 8
5 1 2 3 4
4 5 1 2 3
7 4 5 1 2
Write a program to determine whether a given input is a
Toeplitz
matrix.
Problem 12
Given a positive integer
N
, find the
smallest number of steps it will take to reach
1
.
There are two kinds of permitted steps:
— -> You may
decrement N to N — 1.
— -> If
a * b = N
, you
may decrement
N to the larger of a and b
.
For example, given 100, you can reach 1 in 5 steps with the
following route:100 -> 10 -> 9 -> 3 -> 2 -> 1.
Problem 13
Consider the following scenario: there are
N
mice and
N
holes placed
at integer points along a line. Given this, find a method that
maps mice to holes such that the largest number of steps any
mouse takes is minimized.
Each move consists of moving one mouse
one
unit to the
left
or
right
, and only
one
mouse can
fit inside each hole.
For example, suppose the mice are positioned at
[1, 4, 9, 15]
,
and the holes are located at
[10, -5, 0, 16]
. In this case, the best pairing would require us to send the
mouse at 1
to
the hole at -5
,
so our function should return
6
.
Level Up Coding
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| fct_inorder {forcats} | R Documentation |
This family of functions changes only the order of the levels.
fct_inorder()
: by the order in which they first appear.
fct_infreq()
: by number of observations with each level (largest first)
fct_inseq()
: by numeric value of level.
fct_inorder(f, ordered = NA) fct_infreq(f, ordered = NA) fct_inseq(f, ordered = NA)
f |
A factor |
ordered |
A logical which determines the "ordered" status of the
output factor. |
f <- factor(c("b", "b", "a", "c", "c", "c")) f fct_inorder(f) fct_infreq(f) f <- factor(1:3, levels = c("3", "2", "1")) f fct_inseq(f)


etools-searchable-multiselection-menu demo
Single selection, with search
Multi selection, two lines label
Single Select Menu, two lines label
Multi selection, with search


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Finn Russell Creates & Finishes Amazing Try In Win Over Champions
by Michael CorryRacing 92 rounded off the opening round of the Heineken Champions Cup in style with a 30-10 victory over Saracens in Paris.
It was all one-way traffic from the get-go as the French outfit dominated a largely second-string Saracens from start to finish.
Virimi Vakatawa got Racing off the mark with their first try after nine minutes before Maxime Machenaud added to his earlier penalty to make it 10-0 after 10 minutes.
Machenaud added a further three points before Teddy Thomas sent the Parisians into dreamland after 27 minutes with a second try.
The try was shrouded in controversy over whether the French winger had indeed stepped into touch before finishing.
Draw your own conclusions.
Into the second half and Ben Spencer pulled a try back for Saracens to leave eight between them before Finn Russell conjured up a series of magical moments creating and scoring a wonderful team try that put an end to the Saracens challenge.
Wenceslas Lauret crashed over for the bonus-point try before the end to leave the final score at 30-10 to Racing 92.
The Scotland star, who alluded to their disappointing World Cup in his post-match interview, was in jovial form after a huge opening round victory for the club desperately seeking a first-ever European Champions Cup.


To understand the occurrence of tipping points in periodically forced systems, we take a very simple dynamical system as a useful conceptual model example, where the evolution of state x over time t in this system is determined by
The black lines in Fig. 1a represent this system’s equilibria (dx/dt = 0) for constant D, which we refer to as the equilibrium system. D is an external (prescribed) driver representing environmental conditions, which makes the system non-autonomous (meaning that it explicitly depends on time). In case the driver D changes slowly enough, the system follows a stable equilibrium branch which ends at a bifurcation point. After the driver passes this point the system switches to the remaining stable equilibrium – the case of a classical tipping point.
We now investigate the behavior of the system in response to a driver that oscillates around a mean D m with amplitude D a and period T.
Our conceptual model is hence determined by Eqs 1 and 2, and is well-known as the overdamped limit of the Duffing oscillator. We integrate the system for different sets of the three parameters, D m, D a and T, until it reaches a stable attractor in form of a periodic oscillation. Like the driver, the system’s solution is periodic in time with period T (also involving harmonics that can arise close to a bifurcation point) 17, 18. Figure 2 illustrates how the periodic solutions of the system can change when one of the three parameters is varied. Varying D m (Fig. 2a) is similar to the classical scenario of a tipping point, only that the stable solutions oscillate in time: if D m is increased across the bifurcation, the upper branch of stable solutions disappears and the system has to shift to the lower branch. Interestingly, such tipping-point behavior can also be obtained by increasing the driver’s period T or its amplitude D a, without any change in D m (Fig. 2b–d). For example, when the driver is fast (small T) the system regularly passes the bifurcation point of the equilibrium system but returns in time to keep the system close to the upper branch. Therefore, there can be two alternative periodic solutions. However, when the driver becomes slower, the system destabilizes and propels itself toward the only remaining solution around the lower branch. Figure 2e illustrates this forced transition as a blue trajectory in the phase space spanned by driver D and state x.
Periodic solutions of the conceptual model (Eqs 1 and 2) in dependence on the driver’s mean D m ( a), its period T ( b), and its amplitude D a ( c, d). The blue arrows show the start and end points of linear parameter changes discussed in the text and shown as blue trajectories in ( e, f). The arrows in e-f indicate the overall direction of the change. The two red orbits in each bottom panel are the asymptotic solutions for the parameters at the beginning and end of each transition. See Supplementary Information for details on the parameter choices.
A similar result is obtained when D a is increased (Fig. 2c,f) because the relaxation toward the lower branch becomes too strong. A systematic sampling of the parameter space spanned by D m, D a and T shows that D a and T essentially have a very similar effect in the model (Figs S1, S2) as they both reduce the D m-range in which multiple solutions occur. When both become large, the dependence on initial conditions is destroyed (Fig. S3). This is due to another type of abrupt transition, which occurs at D a = 0.8 in Fig. 2d. At this point, the system reaches a regime where it makes a full cycle involving both branches of the equilibrium system, flipping up and down between the branches (Fig. 2g). As the system’s response becomes very slow at the bifurcation point of the equilibrium system, the transition to the alternative state occurs after the bifurcation point is reached 19. Nonetheless, if the driver’s amplitude is large enough, two abrupt shifts occur within each full cycle of the system under constant parameter conditions. When this regime becomes active, the amplitude of the solution increases rapidly with D a. In contrast to the bifurcations mentioned previously, such sudden amplitude change is reversible: for intermediate D a in Fig. 2d, there are no multiple solutions because all movement occurs along one continuous stable branch far from the second one above. When D a increases, the driver suddenly encloses both bifurcation points. During a cycle, the system now switches to the upper branch, but falls down again later on the other side. It should be noted that the amplitude change is only a sharp transition if T is sufficiently large (compare Fig. 2c with 2d). Otherwise, the time is too short for the system to get close to the alternative branch to which it is suddenly attracted in a short period during each cycle.
This reminds us that Fig. 2a–d displays only asymptotic solutions where the system ends up after an infinite time. In similarity to tipping points in an equilibrium system, the time it takes do make a transition from one to the other solution (blue trajectories in Fig. 2e–g), depends on the response time of the system. This response time can be idealized as a single relaxation time τ. For example, in the equilibrium system given by Eq. 1 and constant D, the relaxation time can be shown to be
The ratio between τ and the driver’s period T determines the abruptness of every one of the transitions discussed above. Three regimes can be distinguished: when T ≫ τ, the system closely follows the stable state of the equilibrium system. This limit case is usually addressed with the classical tipping point concept. When T ≪ τ, the system cannot follow the rapid forcing at all and remains static. It can then be described with an equivalent time-independent system. In the intermediate regime, where the time scales of the system and driver are similar, irreversible amplitude or timescale-induced shifts can occur.


{% extends "includes/main.html" %} {% block title %} This is the homepage {% endblock %} {% block body %} {% include 'includes/plantroom.html' %} {% include 'includes/fishtank.html' %} {% include 'includes/restroom.html' %} {% include 'includes/restaurant.html' %} {% endblock %}


'We need to be ready' - Liverpool fans on whether key man should be risked against Aston Villa
Aston Villa latest - Liverpool fans have been having their say on whether key midfielder Fabinho should start at Villa Park on Saturday.
by Jamie KembleLiverpool fans have been having their say on whether midfielder Fabinho should start against Aston Villa.
The Brazilian is just one booking away from a yellow card with a crucial top-of-the-table clash against Manchester City to come next week.
That means if Fabinho plays and is booked against Villa on Saturday afternoon, he will miss that all-important match-up at Anfield.
Stuck in a dilemma, Jurgen Klopp spoke about the situation in his pre-match press conference.
"I don't know yet," the Liverpool boss replied when asked if he will be risking Fabinho.
Aston Villa latest
This is your round up of all things Villa; the one-stop shop that will keep you updated on the latest goings on at the club and beyond.
Transfers, injuries, match-days and managers, we’ve got you covered.
We’ll be bringing the very latest on the Villains throughout the week and around the clock.
Make sure you keep yourself updated with our handy daily catch up...
Must reads...
- The injury latest on Aston Villa star Jack Grealish - READ
- The team Dean Smith should pick against Wolves - READ
- Darren Bent's message to young striker Keinan Davis - READ
- The referee announced for Liverpool at Villa Park - READ
- The amazing sausage sandwich story Aston Villa fans will love - READ
For all your latest AVFC news, opinion, analysis and transfer gossip, click here
You can follow our Villa reporter Ashley Preece on Twitter, and his email address is<EMAIL_ADDRESS>"We have to see. I know it (the potential suspension), of course. What we do with that I don't know."
But what do Liverpool fans think? Should Fabinho be risked?
Here's what they had to say on Twitter.


--- layout: default title: About slug: about lead: "Learn about the SunPy Project." base_url: "../" ---
The SunPy project is a free and open-source software library for solar physics.
SunPy is a community-developed free and open-source software package for solar physics. SunPy is meant to be a free alternative to the SolarSoft data analysis environment which is based on the IDL scientific programming language sold by Exelis. Though SolarSoft is open-source IDL is not and can be prohibitively expensive. The aim of the SunPy project is to provide the software tools necessary so that anyone can analyze solar data. SunPy is written using the Python programming language and is build upon the scientific Python environment which includes the core packages NumPy, SciPy. The development of SunPy is associated with that Astropy. SunPy was first created in 2011 by a small group of scientists and developers at the NASA Goddard Space Flight Center on nights and weekends.
If you have used SunPy in your scientific work we would appreciate it if you would acknowledge it.
The continued growth and development of SunPy is dependent on the community being aware of the use SunPy. If you use SunPy, we therefore ask that you acknowledge SunPy appropriately in a publication or presentation (poster or talk).
SunPy is an alternative to the popular SolarSoft analysis environment
The IDL-based SolarSoft analysis environment is a mature and rich code base to do Solar physics. Unfortunately not every person or institution have the capital necessary to fund a yearly IDL license. With the rise of scientific computing in Python new tools are now available to make developing the basics of a solar data analysis environment straightforward.
SunPy is a living code base with many contributors. Anyone can and is welcome to get involved.
SunPy is maintained and developed by the founding team and a group of core contributors and organizers. SunPy has also had received funding from and hosted students interns from the Google Summer of Code and the European Space Agency Summer of Code
Get involved with SunPy development by opening an issue or submitting a pull request.
The core team is composed of the following members (in alphabetical order)
If you think you belong on this list please send an the mailing list or make a pull request and add yourself!
Stay up to date on the development of SunPy and interact with the community with these helpful resources.
irc.freenode.net
server, in the #sunpy channel.Looking forward to meeting you!
Part of SunPy has been developed with help from the Google and ESA Summer of Code programs.
Part of the development of SunPy has been generously supported by the Google Summer of Code (GSOC) as well as the European Space Agency Summer of Code in Space (SOCIS). Both of these programs have funded several students to work on SunPy for a few months (usually during the summer).
SunPy would like to thank both of these programs for their support.


Description:
The calculator combines a calculator for eGFR-MDRD (1,2,3) and a calculator for kineticGFR (4).
The following variables significantly affect calculated outputs:
- Choice of GFR estimator affects GFR calculations. MDRD was used in reference to Chen et al. (4).
- According to the National Kidney Foundation, laboratories should now be using a creatinine method that has been standardized or tracable to isotope dilution mass spectrometry (IDMS). The way creatinine levels are calibrated affects the GFR estimating equation. (3)
- The creatinine measurement unit (μmol/L versus mg/dL) affects the GFR estimating equation. Creatinine levels in μmol/L are converted to mg/dL in our calculator by dividing them by 88.4. (5)
- The value maximal rise in plasma creatinine per day is ambiguous. See Chen et al. for a discussion of this topic. (4)
References:
- A more accurate method to estimate glomerular filtration rate from serum creatinine: a new prediction equation. Modification of Diet in Renal Disease Study Group. Levey AS, Bosch JP, Lewis JB, Greene T, Rogers N, Roth D. Ann Intern Med. 1999 Mar 16;130(6):461-70. PMID: 10075613 [PubMed - indexed for MEDLINE]
- Levey A, Greene T, Kusek J, Beck G, Group MS. A simplified equation to predict glomerular filtration rate from serum creatinine. J Am Soc Nephrol 2000;11:155A
- Expressing the Modification of Diet in Renal Disease Study equation for estimating glomerular filtration rate with standardized serum creatinine values. Levey AS, Coresh J, Greene T, Marsh J, Stevens LA, Kusek JW, Van Lente F; Chronic Kidney Disease Epidemiology Collaboration. Clin Chem. 2007 Apr;53(4):766-72. Epub 2007 Mar 1. PMID: 17332152 [PubMed - indexed for MEDLINE]
- Retooling the creatinine clearance equation to estimate kinetic GFR when the plasma creatinine is changing acutely. Chen S. J Am Soc Nephrol. 2013 May;24(6):877-88. doi: 10.1681/ASN.2012070653. Epub 2013 May 23. PMID: 23704286 [PubMed - indexed for MEDLINE]
- http://en.wikipedia.org/w/index.php?title=Renal_function&oldid=624916087
Disclaimer:
All information is provided for educational purposes only.
This information should not be used for the diagnosis or treatment of any health problem or disease.
THIS INFORMATION IS NOT INTENDED TO REPLACE CLINICAL JUDGMENT OR GUIDE INDIVIDUAL PATIENT CARE IN ANY MANNER.
We'd love to hear your comments!
This is an open source project that can be contributed to.
v 0.0.4


Blacksmith Poitan:
Oh, Barbado. What would he want?
Oh, I know! He mentioned recently that he wanted to learn a new instrument! Burp! Perhaps what he wants is a flute!


Current research interests include advanced power generation systms (e.g., oxy-fuel combustion, chemical looping), radiative heat transfer, and multi-physics simulations.
Bradley Adams joined BYU in 2015 after 30 years in industry, including positions at GenRad, MIT Lincoln Laboratories, and Reaction Engineering International. He has significant experience in technical management and has performed R&D in the areas of heat transfer, combustion, and air pollution control, with an emphasis on CFD simulation of these processes.
Bradley Adams joined BYU in 2015 after 30 years in industry, including positions at GenRad, MIT Lincoln Laboratories, and more.
Dr. Ames has been at Brigham Young University since fall 2012. Previously he was an Associate Professor at Idaho State University and a Research Assistant Professor at Utah State University. Dr. Ames is the original developer and project manager of several open source GIS based software tools including the widely used MapWindow GIS (www.mapwindow.org), DotSpatial Library (www.dotspatial.org) and HydroDesktop data management system (www.hydrodesktop.org). Dr. Ames’ research interests and publications include geospatial and hydrologic web services, hydrologic information systems, probabilistic watershed modeling, uncertainty characterization, terrain analysis, evapotranspiration, immersive virtual reality visualization, and open hardware data sensor networks. Dr. Ames has conducted and overseen numerous GIS and engineering software development projects funded by NSF, EPA, USGS, and various state and local agencies and private industry.
Embedded systems, computer vision, real-time systems
Dr. Archibald received the BS degree in mathematics from BYU in 1981, and MS and PhD degrees in computer science from the University of Washington in 1983 and 1987 respectively. He has been with BYU's Electrical and Computer Engineering Department since 1987. In 1994-1995 he was a visiting professor at the Swiss Federal Institute of Technology in Zurich. Dr. Archibald's current research interests are in the areas of real-time computer vision systems and autonomous agents.
Bradley Adams joined BYU in 2015 after 30 years in industry, including positions at GenRad, MIT Lincoln Laboratories, and Reaction Engineering International. He has significant experience in technical management and has performed R&D in the areas of heat transfer, combustion, and air pollution control, with an emphasis on CFD simulation of these processes. Current research interests include advanced power generation systms (e.g., oxy-fuel combustion, chemical looping), radiative heat transfer, and multi-physics simulations.
Current research interests include advanced power generation systms (e.g., oxy-fuel combustion, chemical looping), radiative heat transfer, and multi-physics simulations.
Fossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2bFossil Fuels, Encyclopedia of Sustainability Science and Technology; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 85b; 2015 Spring Meeting & 11th Global Congress on Process Safety: Paper 2b
Todd Williams (PhD), Taylor Schroedter (MS)
ME 510 - Compressible Flow; ME 340 - Heat Transfer; ME 393 - Professional Skills
Most Important, Original, and High Quality Paper ASPACC-99 (Combustion Institute) 1999
This is a card that can be used for custom content.
This is where the faculty education goes!
This is where the CV goes!


First year HCI DM Track Masters candidate at Georgia Tech, Yvonne is an avid animal lover and art enthusiastic. One of the animals that brings her most joy is the husky puppy. Fluffy puppies will brighten anyone's day and hoards of puppy pictures will whisk you away to happier places.
When she is not working hard to spur on her WebDev/UX/UI career or looking at cute puppers, she loves to explore local art galleries and revel in the works of masters across many ages. Can you guess from her portrait what one of her favorite pieces is?
First year DM Masters candidate at Georgia Tech, Grace is a quirky squirrel and cat lover who enjoys making of all kinds, from crafting to learning a little coding. One of the biggest bonuses of moving from a small town to a bit city meant that there were more galleries and art museums to explore.
Although she is not contemporary art's biggest fan, she values the exposure to current artists and their works and enjoys novel experiences. That being said, it is always nice to know what local galleries might be housing pieces from gothic or romantic periods. If you ask her who her favorite artist is, she would give you a list of artists that have nothing in common, save that they evolved over time and shamelessly created controversial content simply because they wanted to and saw beauty beyond what was trending at their time. Long live the revolutionaries and long live squirrels!


Blockchain for Business
WITH IBM BLOCKCHAIN
TRACK & TRACE
Home
Manufacturer
Distributor
Dealer
Hospital
Dashboard
Dashboard
UUID


Perhaps @mzelesky or @kevinreiss could take a look at this one
@christinach @kevinreiss temp access hathi. Ready for re-review.
mentioned
by Kevin Reiss at 2021-04-09 12:43:21.subscribed
by Kevin Reiss at 2021-04-09 12:43:21.mentioned
by None at 2021-04-09 12:43:21.subscribed
by None at 2021-04-09 12:43:21.review_dismissed
by Eliot Jordan at 2021-04-09 14:34:49.mentioned
by Kevin Reiss at 2021-04-09 14:35:47.subscribed
by Kevin Reiss at 2021-04-09 14:35:47.mentioned
by Christina Chortaria at 2021-04-09 14:35:51.subscribed
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by Christina Chortaria at 2021-04-09 14:49:01.closed
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by Christina Chortaria at 2021-04-09 14:49:01.referenced
by Christina Chortaria at 2021-04-09 16:06:23.merged
by Christina Chortaria at 2021-04-09 16:06:23.closed
by Christina Chortaria at 2021-04-09 16:06:23.head_ref_deleted
by Christina Chortaria at 2021-04-09 16:06:24.labeled
by Christina Chortaria at 2021-04-09 16:31:39.mentioned
by None at 2021-04-09 16:31:39.subscribed
by None at 2021-04-09 16:31:40.mentioned
by Christina Chortaria at 2021-04-09 15:10:31.subscribed
by Christina Chortaria at 2021-04-09 15:10:31.referenced
by Christina Chortaria at 2021-04-09 16:06:41.merged
by Christina Chortaria at 2021-04-09 16:06:41.closed
by Christina Chortaria at 2021-04-09 16:06:41.head_ref_deleted
by Christina Chortaria at 2021-04-09 16:06:41.head_ref_force_pushed
by Christina Chortaria at 2021-04-09 15:35:01.head_ref_force_pushed
by Christina Chortaria at 2021-04-09 16:41:20.I'm sorry @tpendragon this needs a rebase
mentioned
by Trey Pendragon at 2021-04-09 16:07:24.subscribed
by Trey Pendragon at 2021-04-09 16:07:24.head_ref_force_pushed
by Trey Pendragon at 2021-04-09 17:02:47.assigned
by Trey Pendragon at 2021-04-09 17:30:39.closed
by Eliot Jordan at 2021-04-09 17:30:41.assigned
by James R. Griffin III at 2021-04-09 18:28:42.unlabeled
by None at 2021-04-09 18:42:48.Otherwise, this may be resolved as part of #1204
In production: https://catalog.princeton.edu/catalog/1414145/raw In holdings1display, the MFHD ID has copynumber.
This record is not indexed in catalog-alma-qa.
assigned
by None at 2021-04-09 15:17:54.referenced
by None at 2021-04-09 15:50:19.closed
by None at 2021-04-09 20:34:44.assigned
by None at 2021-04-09 15:07:16.referenced
by None at 2021-04-09 15:09:22.closed
by None at 2021-04-09 20:37:56.review_dismissed
by None at 2021-04-09 20:35:55.referenced
by Trey Pendragon at 2021-04-09 20:51:55.merged
by Trey Pendragon at 2021-04-09 20:51:56.closed
by Trey Pendragon at 2021-04-09 20:51:56.head_ref_deleted
by Trey Pendragon at 2021-04-09 20:51:56.closed
by Kevin Reiss at 2021-04-09 14:41:32.closed
by Kevin Reiss at 2021-04-09 14:42:29.referenced
by Kevin Reiss at 2021-04-09 16:23:07.merged
by Kevin Reiss at 2021-04-09 16:23:07.closed
by Kevin Reiss at 2021-04-09 16:23:07.head_ref_deleted
by Kevin Reiss at 2021-04-09 16:23:21.This is probably because it's keywordsssim vs keywordstesim.
added_to_project
by None at 2021-04-09 17:41:07.added_to_project
by None at 2021-04-09 20:45:30.labeled
by None at 2021-04-09 20:45:55.Yeah I think this is a side effect of grouping DPUL does.
Can we just get rid of this? Next/previous is really buggy in general for Blacklight, especially with things like multiple tabs.
What would we have in lieu of it?
I usually just use the browser back button and go to the next thing, or use browser tabs
hmm.
Ellen and I have reviewed the previous/next issues. and have found different functionality depending on how you navigate to different groupings of the collection. BROWSE: in browse category, you have no next/previous option from the list, but when you select the item you do have the next/previous option--which doesn't work at all well. Mirroring this.....
FACETS from home page (by provenance, for example): you have the option to use next/previous in list search display, that seems to function appropriately (when something other than "relevance" is selected for sorting). But when you select an item from the list search display, the option for previous/next disappears.
If we had a choice, the browse categories would mirror the facets search, in terms of the previous/next buttons. This would be seen as the best option available right now, but something we would like to revisit when the 3.0 upgrade happens. Are you intending to just remove the item level previous/next, @tpendragon and @hackartisan ?
mentioned
by None at 2021-04-09 20:47:38.subscribed
by None at 2021-04-09 20:47:38.mentioned
by Trey Pendragon at 2021-04-09 20:47:38.subscribed
by Trey Pendragon at 2021-04-09 20:47:38.labeled
by Kevin McElwee at 2021-04-09 15:59:43.assigned
by Kevin McElwee at 2021-04-09 15:59:43.closed
by Kevin McElwee at 2021-04-09 16:04:50.closed
by Kevin McElwee at 2021-04-09 17:35:49.referenced
by Kevin McElwee at 2021-04-09 17:35:49.merged
by Kevin McElwee at 2021-04-09 17:35:49.closed
by Kevin McElwee at 2021-04-09 17:35:50.No discrepency has been raised in three months, closing for now
closed
by Kevin McElwee at 2021-04-09 18:20:22.labeled
by Esmé Cowles at 2021-04-09 19:12:12.deployed
by Trey Pendragon at 2021-04-09 14:49:59.deployed
by Trey Pendragon at 2021-04-09 15:37:50.renamed
by Francis Kayiwa at 2021-04-09 21:01:22.referenced
by Bess Sadler at 2021-04-09 21:02:36.merged
by Bess Sadler at 2021-04-09 21:02:36.closed
by Bess Sadler at 2021-04-09 21:02:36.head_ref_deleted
by Bess Sadler at 2021-04-09 21:02:37.referenced
by Kevin Reiss at 2021-04-09 13:48:49.merged
by Kevin Reiss at 2021-04-09 13:48:49.closed
by Kevin Reiss at 2021-04-09 13:48:49.head_ref_deleted
by Kevin Reiss at 2021-04-09 13:48:49.Closing duplicate
review_requested
by Kevin Reiss at 2021-04-08 23:39:50.closed
by Kevin Reiss at 2021-04-09 13:49:03.head_ref_force_pushed
by None at 2021-04-09 14:23:52.head_ref_force_pushed
by None at 2021-04-09 19:17:17.referenced
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by Kevin Reiss at 2021-04-09 17:05:54.head_ref_deleted
by Kevin Reiss at 2021-04-09 17:06:07.head_ref_deleted
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by Kevin Reiss at 2021-04-09 17:06:13.head_ref_deleted
by Kevin Reiss at 2021-04-09 17:06:16.closed
by Kevin Reiss at 2021-04-09 19:36:04.reopened
by Kevin Reiss at 2021-04-09 19:36:07.renamed
by Kevin Reiss at 2021-04-09 19:36:30.@carolyncole I think we can close this one.
mentioned
by None at 2021-04-09 19:36:56.subscribed
by None at 2021-04-09 19:36:56.closed
by Axa Mei Liauw at 2021-04-09 14:43:59.assigned
by Shaun Ellis at 2021-04-09 14:48:26.renamed
by Axa Mei Liauw at 2021-04-09 14:48:42.referenced
by Kevin McElwee at 2021-04-09 20:03:32.merged
by Kevin McElwee at 2021-04-09 20:03:32.closed
by Kevin McElwee at 2021-04-09 20:03:32.head_ref_deleted
by Kevin McElwee at 2021-04-09 20:03:33.


Ondo FRSC Warns Officers Against Bribery
In terms of taking bribe or compromising, I always tell our officers that any money taken on the highway is ‘blood money’.
by SaharaReporters, New YorkThe Federal Road Safety Corps in Ondo State has warned its officers manning federal highways against taking bribes from traffic offenders.
Commander of FRSC in the state, Rotimi Adeleye, sounded the note of warning to the officers on Thursday while speaking with journalists in Akure, the state capital.
According to Adeleye, any officer demanding bribe from traffic offenders was asking for 'blood money'.
He said, “In terms of taking bribe or compromising, I always tell our officers that any money taken on the highway is ‘blood money’.
“Taking money from someone that is speeding means that you are giving them liberty to cause accident.”
Speaking further, Adeleye urged vehicle owners to adhere to driving rules so as to avoid road crashes especially at this time of the year when the festive season was fast approaching.


Either a string or a callback that returns a string for the phone to use to login.
callback that should return the login code that telegram sent.
has optional bool isCodeViaApp
param for whether the code was sent through the app (true) or an SMS (false).
optional string or callback that should return the 2FA password if present.
the password hint will be sent in the hint param
in case of a new account creation this callback should return a first name and last name [first,last]
.
a qrCode token for login through qrCode.
this would need a QR code that you should scan with another app to login with.
when an error happens during auth this function will be called with the error.
if this returns true the auth operation will stop.
whether to send the code through SMS or not.
Generated using TypeDoc
For when you want to login as a Api.User
this should handle all needed steps for authorization as a user.
to stop the operation at any point just raise and error with the message
AUTH_USER_CANCEL
.


To start the tests click Start. Each test is run in order (downloaded from the server). Tests are run for a maximum number of frames (specified below), and the time recorded.


A suite of conversion scripts to create internally standardized
spatial polygons data frames. Utility scripts use these data sets to return
values such as country, state, timezone, watershed, etc. associated with a
set of longitude/latitude pairs. (They also make cool maps.)
| Version: |
0.5.4 |
| Depends: |
R (≥ 3.1.0), sp |
| Imports: |
dplyr, lubridate, rgdal, rgeos, rmapshaper, rvest (≥ 0.3.0), stringr, utils, xml2 |
| Suggests: |
knitr, maps, markdown, readr, testthat |
| Published: |
2018-09-18 |
| Author: |
Jonathan Callahan [aut, cre],
Ruby Fore [aut],
Will Leahy [aut],
Helen Miller [aut],
Henry Nguyen [aut],
Robin Winstanley [aut],
Alice Yang [aut] |
| Maintainer: |
Jonathan Callahan <jonathan.s.callahan at gmail.com> |
| License: |
GPL-2 |
| NeedsCompilation: |
no |
| Materials: |
README |
| CRAN checks: |
MazamaSpatialUtils results |


Latest Pictures on Flickr
Features We're Building
Multimedia Management Features
Support for multimedia uploading and management for engaging students; to simplify a task that would otherwise be a major technical hurdle.
Enrichment Features
Teachers and administrators can enrich existing data with semi-automated metadata.
Translation Features
This feature includes all aspects of managing an incoming queue of translation requests including job prioritization, translator reputation, job queuing and locking, content versioning, translation ranking, translation permissioning, translator payments.
Sharing Features
Teachers can share resources including links, documents, essays, extracts, citations, abstracts, taxonomies, curricula, primary sources, blog posts, annotated web pages, video, photos, conversation logs. This feature can be expressed in a number of ways across a variety of platforms, including social media sharing but also more general wiki write-ups, or streamlined resources bundling and sharing.
Study Features
This set of features includes aspects of study such as flashcards, drills and quizzes.
Profile Features
Profile Creation and Management including avatar uploading, background and summary of interests, links to existing pages about each user of the site; for insight into teacher context.
Discussion Features
Teachers can message and comment to each other in translated dialogue about various objects in the system; to gain support for
Rating Features
The teachers are able to rate content as being superior or inferior, probably on a simple scale of 0-3 stars; to help filtering of diverse information to capture what is relevant for busy teachers.
Content and Concept Mapping Features
The content and concept mapping feature for organizing instructional materials for individual courses or entire curricula, creating educational resources, to visualize lessons, consolidate and educational topics in both nonlinear (eg, concept maps) and linear ways (eg, calendaring).
Tools We Use
Delicious
Delicious is a Yahoo-owned, web-based tool for tagging URLs on the web.
Epsilen
Epsilen is a multifaceted tool for managing groups, wikis and conversations.
Atlas
Atlas is a tool for mapping curriculum.
Twitter is a "microblogging" tools for forming networks and sending short status updates.
Ibis
Ibis is a platform for translated conversation.
YouTube
YouTube is a Google-Owned, web-based platform for sharing video and commenting.
YALLAH
YALLAH is a form for cross language discussion
Facebook is a popular tool for sharing text updates and multimedia to groups and the public.
Flickr
Flickr is a tool for managing photos and videos, and for forming groups around archives.
VUE
The Visual Understanding Environment (VUE) is an Open Source project based at Tufts University. The VUE project is focused on creating flexible tools for managing and integrating digital resources in support of teaching, learning and research. VUE provides a flexible visual environment for structuring, presenting, and sharing digital information.


Join Us. Easy accessability of all the handyman data. Book according to your comfort. Rate the handyman. Be insured with us
Join Us. Easy accessability of all the handyman data. Contract handyman according to your need. Rate the handyman. Be insured with us.