Skip to main content

Due to the lapse in federal government funding, NASA is not updating this website. We sincerely regret this inconvenience.

Xspec Home Page

next up previous contents
Next: sedov, vsedov, vvsedov, bsedov, Up: Additive Model Components Previous: rsgauss: gaussian line profile   Contents


rsrnei, rsvrnei, rsvvrnei: Non-equilibrium recombining collisional plasma with resonance scattering

A version of the rnei model modified by resonance scattering out of the beam following Chakraborty et al. (2023). This assumes the entire observed beam is described by this model and there is no significant scattering into the beam. The free parameter for the resonance scattering is the column in units of 10$^{22}$ cm$^{-2}$. This model also includes a velocity broadening parameter and includes thermal broadening of all lines. The calculated line shape includes the different resonance scattering correction between the core and the wings. For large columns this can produce a double-peaked structure.

See the rnei model for information about the additional options available.

For the rsrnei model the parameters are:

par1 Plasma temperature (keV)
par2 Initial plasma temperature (keV)
par3 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
par4 Ionization timescale in units of s/cm$^3$.
par5 redshift
par6 gaussian velocity broadening (sigma in km/s)
par7 resonance scattering column ($10^{22}$ cm${^-2}$)
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 rsvrnei variant the parameters are as follows.

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
par18 gaussian velocity broadening (sigma in km/s)
par19 resonance scattering column ($10^{22}$ cm${^-2}$)
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 rsvvrnei variant the parameters are as follows.

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
par35 gaussian velocity broadening (sigma in km/s)
par36 resonance scattering column ($10^{22}$ cm${^-2}$)
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
next up previous contents
Next: sedov, vsedov, vvsedov, bsedov, Up: Additive Model Components Previous: rsgauss: gaussian line profile   Contents