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meka, vmeka: emission, hot diffuse gas (Mewe-Gronenschild)

An emission spectrum from hot diffuse gas based on the model calculations of Mewe and Gronenschild (as amended by Kaastra). The model includes line emissions from several elements. Abundances are the number of nuclei per Hydrogen nucleus relative to the Solar abundances set by the abund command.

For the meka model the parameters are:

par1 plasma temperature in keV
par2 H density (cm$^{-3}$
par3 Metal abundances (He fixed at cosmic). The elements included are C, N, O, Ne, Na, Mg, Al, Si, S, Ar, Ca, Fe, Ni. Relative abundances are set by the abund command.
par4 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), $n_e$ and $n_H$ are the electron and H densities (cm$^{-3}$), respectively

For the vmeka variant the parameters are as follows.

par1 plasma temperature in keV
par2 H density (cm$^{-3}$
par3-par14 Abundances for He, C, N, O, Ne, Mg, Si, S, Ar, Ca, Fe, Ni wrt Solar (defined by the abund command).
par15 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), $n_e$ and $n_H$ are the electron and H densities (cm$^{-3}$), respectively

The references for the meka model are as follows :
Mewe, R., Gronenschild, E.H.B.M., and van den Oord, G.H.J. 1985 A&AS, 62, 197
Mewe, R., Lemen, J.R., and van den Oord, G.H.J. 1986, A&AS, 65, 511
Kaastra, J.S. 1992, An X-Ray Spectral Code for Optically Thin Plasmas (Internal SRON-Leiden Report, updated version 2.0)

Similar credit may also be given for the adopted ionization balance:
Arnaud, M., and Rothenflug, M. 1985, A& AS, 60, 425
Arnaud, M., and Raymond, J. 1992, ApJ, 398, 394


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Next: mekal, vmekal: emission, hot Up: Additive Model Components Previous: lorentz: lorentz line profile