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gnei, vgnei, vvgnei: 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
3.0 ionization fractions and spectrum calculation uses AtomDB v3

Note that versions 1.x have no emission from Ar. The default is version 3.0. The vgnei variant allows the user to set the abundances for the more common elements. For versions 3 and above the abundances of the trace elements (ie Li, Be, B, F, Na, P, Cl, K, Sc, Ti, V, Cr, Mn, Co, Cu, Zn) can be set using xset APEC_TRACE_ABUND. These trace element abundances can be set either to the abundance of one of the main elements or to a numerical value (relative to Solar). For instance,

XSPEC12> xset APEC_TRACE_ABUND Fe
sets trace element abundances to that of iron while
XSPEC12> xset APEC_TRACE_ABUND 1.0
sets them to Solar. The default value for APEC_TRACE_ABUND is 1.0. Full control over all the elemental abundances is available in the vvgnei model.

For the gnei model the parameters are:

par1 plasma temperature (keV)
par2 Metal abundances (He fixed at cosmic). 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 $(10^{-14}/(4\pi[D_A(1+z)]^2))\int n_en_H dV$, where $D_A$ is the angular diameter distance to the source (cm), $n_e$ is the electron density (cm$^{-3}$), and $n_H$ is the hydrogen density (cm$^{-3}$).

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 $(10^{-14}/(4\pi[D_A(1+z)]^2))\int n_en_H dV$, where $D_A$ is the angular diameter distance to the source (cm), $n_e$ is the electron density (cm$^{-3}$), and $n_H$ is the hydrogen density (cm$^{-3}$).

Finally, 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 $(10^{-14}/(4\pi[D_A(1+z)]^2))\int n_en_H dV$, where $D_A$ is the angular diameter distance to the source (cm), $n_e$ is the electron density (cm$^{-3}$), and $n_H$ is the hydrogen density (cm$^{-3}$).


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Next: grad: accretion disk, Schwarzschild Up: Additive Model Components Previous: gauss, zgauss: gaussian line