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rnei, vrnei, vvrnei: non-equilibrium recombining collisional plasma

Non-equilibrium ionization collisional plasma model. This is a beta test version of a model for a recombining plasma where the plasma is assumed to have started in collisional equilibrium with the initial temperature given by the relevant input parameter. This model will only work for xset neivers 3.0 and above. The default is 3.0.

The vrnei variant allows the user to set the abundances of the most common elements. 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 vvrnei model.

For the rnei model the parameters are:

par1 Plasma temperature (keV)
par2 Initial plasma temperature (keV)
par3 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
par4 Ionization timescale in units of s/cm$^3$.
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 vrnei model, the parameters are:

par1 Plasma temperature (keV)
par2 Initial plasma temperature (keV)
par3 H abundance (set to 0 for no free-free continuum, otherwise 1)
par4-par15 Abundances for He, C, N, O, Ne, Mg, Si, S, Ar, Ca, Fe, Ni wrt Solar (defined by the abund command)
par16 Ionization timescale in units of s/cm$^3$.
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 vvrnei model, the parameters are:

par1 Plasma temperature (keV)
par2 Initial plasma temperature (keV)
par3 H abundance (set to 0 for no free-free continuum, otherwise 1)
par4-par32 Abundances for all elements with 2 $\leq$ Z $\leq$ 30 wrt Solar (defined by the abund command)
par33 Ionization timescale in units of s/cm$^3$.
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$^{-3}$).


next up previous contents
Next: sedov, vsedov, vvsedov: sedov Up: Additive Model Components Previous: refsch: reflected power law