This model interpolates from a grid of neutron star (NS) atmosphere spectra to produce a final spectrum that depends on the parameters listed below. The atmosphere spectra are obtained using the latest equation of state and opacity results for a partially ionized, strongly magnetized hydrogen or mid-Z element plasma. The models are constructed by solving the coupled radiative transfer equations for the two photon polarization modes in a magnetized medium, and the atmosphere is in radiative and hydrostatic equilibrium. The atmosphere models mainly depend on the surface effective temperature Teff and magnetic field strength B and inclination ΘB; there is also a dependence on the surface gravity g=(1+zg)GM/R2, where 1+zg=(1-2GM/R)-1/2 is the gravitational redshift and M and R are the NS mass and radius, respectively.
Two sets of models are given: one set with a single surface B and Teff and a set which is constructed with B and Teff varying across the surface according to the magnetic dipole model (for the latter, θm is the angle between the direction to the observer and the magnetic axis). The effective temperatures span the range log Teff=5.5-6.8 for hydrogen and log Teff.=5.8-6.9 for mid-Z elements(note: for the latter, change temperature range in nsmax_lmodel.dat) The models with single (B,Teff) cover the energy range 0.05-10 keV, while the models with (B,Teff)-distributions cover the range 0.09-5 keV.
par1 = logTeff, surface (unredshifted) effective temperature
par2 = 1+zg, gravitational redshift
par3 = switch indicating model to use (see nsmax.dat or model list)
A = (Rem/d)2, normalization, where Rem is the size (in km) of the emission region and d is the distance (kpc) to the object Note: A is added automatically by XSPEC.
Please send your comments/questions to Wynn Ho (firstname.lastname@example.org). If you publish results obtained using NSMAX, please reference Ho, W.C.G., Potekhin, A.Y., & Chabrier, G. (2008, ApJS, 178, 102) and also Mori, K. & Ho, W.C.G. (2007, MNRAS, 377, 905) if using the mid-Z models.