Skip to main content

To find and download HEASARC data in the cloud, you can use astroquery.heasarc or download our new tool, hark.

The HEASARC and NuSTAR teams are greatly saddened by the sudden passing of Katja Pottschmidt. Most recently Katja was the lead scientist for the NuSTAR Guest Observer Facility (GOF), a role she had supported for many years. During her science career she worked on many other high energy astrophysics missions and played an integral role in advancing our knowledge of the universe. She was a wonderful colleague and friend and will be keenly missed by all who knew her.

next up previous contents
Next: sedov, vsedov, vvsedov, bsedov, Up: Additive Model Components Previous: relline, relline_lp, relline_lp_ext: relativistic   Contents


rnei, vrnei, vvrnei, brnei, bvrnei, bvvrnei: non-equilibrium recombining collisional plasma

Non-equilibrium ionization collisional plasma model. This is 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. Additional xset options are available and are listed under the documentation for nei.

For the rnei 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
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 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 ${10^{-14}\over{4\pi[D_A(1+z)]^2}}\int n_en_HdV$, 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 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 ${10^{-14}\over{4\pi[D_A(1+z)]^2}}\int n_en_HdV$, 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 brnei 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)
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 bvrnei 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
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 bvvrnei 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
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

next up previous contents
Next: sedov, vsedov, vvsedov, bsedov, Up: Additive Model Components Previous: relline, relline_lp, relline_lp_ext: relativistic   Contents