gnei, vgnei, vvgnei, bgnei, bvgnei, bvvgnei: collisional plasma, non-equilibrium, temperature evolution

Non-equilibrium ionization collisional plasma model. This is a generalization of the nei model where the temperature is allowed to have been different in the past i.e. the ionization timescale averaged temperature is not necessarily equal to the current temperature. For example, in a standard Sedov model with equal electron and ion temperatures, the ionization timescale averaged temperature is always higher than the current temperature for each fluid element. The references for this model can be found under the description of the equil model. Several versions are available. To switch between them use the xset neivers command. The versions available are:

1.0	the version from xspec v11.1
1.1	as 1.0 but with updated ionization fractions using dielectronic recombination rates from Mazzotta et al. (1998)
2.0	same ionization fractions as 1.1 but uses AtomDB v2 to calculate the resulting spectrum
3.x	ionization fractions and spectrum calculation uses AtomDB v3.x

Note that versions 1.x have no emission from Ar. For versions 3.x and later additional xset options are available and are listed under the documentation for nei.

For the gnei model the parameters are:

par1	plasma temperature (keV)
par2	Metal abundances (He fixed at that defined by the abund command). The elements included are C, N, O, Ne, Mg, Si, S, Ar, Ca, Fe, Ni. Abundances are defined by the abund command
par3	Ionization timescale in units of s/cm$^3$.
par4	Ionization timescale averaged plasma temperature (keV)
par5	redshift
norm	${10^{-14}\over{4\pi[D_A(1+z)]^2}}\int n_en_HdV$, where $D_A$ is the angular diameter distance to the source (cm), $dV$ is the volume element (cm$^3$), and $n_e$ and $n_H$ are the electron and H densities (cm$^{-3}$), respectively

For the vgnei model, the parameters are:

par1	plasma temperature (keV)
par2	H abundance (set to 0 for no free-free continuum, otherwise 1)
par3–par14	Abundances for He, C, N, O, Ne, Mg, Si, S, Ar, Ca, Fe, Ni wrt Solar (defined by the abund command)
par15	Ionization timescale in units of s/cm$^3$.
par16	Ionization timescale averaged plasma temperature (keV)
par17	Redshift, z
norm	${10^{-14}\over{4\pi[D_A(1+z)]^2}}\int n_en_HdV$, where $D_A$ is the angular diameter distance to the source (cm), $dV$ is the volume element (cm$^3$), and $n_e$ and $n_H$ are the electron and H densities (cm$^{-3}$), respectively

For the vvgnei model, the parameters are:

par1	plasma temperature (keV)
par2	H abundance (set to 0 for no free-free continuum, otherwise 1)
par3–par31	Abundances for all elements with 2 $\leq$ Z $\leq$ 30 wrt Solar (defined by the abund command)
par32	Ionization timescale in units of s/cm$^3$.
par33	Ionization timescale averaged plasma temperature (keV)
par34	Redshift, z
norm	${10^{-14}\over{4\pi[D_A(1+z)]^2}}\int n_en_HdV$, where $D_A$ is the angular diameter distance to the source (cm), $dV$ is the volume element (cm$^3$), and $n_e$ and $n_H$ are the electron and H densities (cm$^{-3}$), respectively

For the bgnei model the parameters are:

par1	plasma temperature (keV)
par2	Metal abundances (He fixed at that defined by the abund command). The elements included are C, N, O, Ne, Mg, Si, S, Ar, Ca, Fe, Ni. Abundances are defined by the abund command
par3	Ionization timescale in units of s/cm$^3$.
par4	Ionization timescale averaged plasma temperature (keV)
par5	redshift
par6	gaussian velocity broadening (sigma in km/s)
norm	${10^{-14}\over{4\pi[D_A(1+z)]^2}}\int n_en_HdV$, where $D_A$ is the angular diameter distance to the source (cm), $dV$ is the volume element (cm$^3$), and $n_e$ and $n_H$ are the electron and H densities (cm$^{-3}$), respectively

For the bvgnei model, the parameters are:

par1	plasma temperature (keV)
par2	H abundance (set to 0 for no free-free continuum, otherwise 1)
par3–par14	Abundances for He, C, N, O, Ne, Mg, Si, S, Ar, Ca, Fe, Ni wrt Solar (defined by the abund command)
par15	Ionization timescale in units of s/cm$^3$.
par16	Ionization timescale averaged plasma temperature (keV)
par17	Redshift, z
par18	gaussian velocity broadening (sigma in km/s)
norm	${10^{-14}\over{4\pi[D_A(1+z)]^2}}\int n_en_HdV$, where $D_A$ is the angular diameter distance to the source (cm), $dV$ is the volume element (cm$^3$), and $n_e$ and $n_H$ are the electron and H densities (cm$^{-3}$), respectively

Finally, for the bvvgnei model, the parameters are:

par1	plasma temperature (keV)
par2	H abundance (set to 0 for no free-free continuum, otherwise 1)
par3–par31	Abundances for all elements with 2 $\leq$ Z $\leq$ 30 wrt Solar (defined by the abund command)
par32	Ionization timescale in units of s/cm$^3$.
par33	Ionization timescale averaged plasma temperature (keV)
par34	Redshift, z
par35	gaussian velocity broadening (sigma in km/s)
norm	${10^{-14}\over{4\pi[D_A(1+z)]^2}}\int n_en_HdV$, where $D_A$ is the angular diameter distance to the source (cm), $dV$ is the volume element (cm$^3$), and $n_e$ and $n_H$ are the electron and H densities (cm$^{-3}$), respectively

HEASARC Home | Observatories | Archive | Calibration | Software | Tools | Students/Teachers/Public

Last modified: Friday, 23-Aug-2024 13:20:40 EDT

HEASARC Staff Scientist Position - Applications are now being accepted for a Staff Scientist with significant experience and interest in the technical aspects of astrophysics research, to work in the High Energy Astrophysics Science Archive Research Center (HEASARC) at NASA Goddard Space Flight Center (GSFC) in Greenbelt, MD. Refer to the AAS Job register for full details.