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nsmaxg: Neutron Star with a Magnetic Atmosphere

The nsmaxg model interpolates from a grid of neutron star (NS) atmosphere spectra to produce a final spectrum that depends on the parameters listed below. 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. 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. Atmosphere models mainly depend on the surface effective temperature $T_{eff}$ and magnetic field strength $B$ and inclination $\Theta_B$; there is also a dependence on the surface gravity $g = (1+z_g)GM/R^2$, where $1+z_g = 1/\sqrt{1-2GM/R}$ is the gravitational redshift and $M$ and $R$ are the NS mass and radius, respectively.

Two sets of models are available: one set with a single surface $B$ and $T_{eff}$ [some models allow for varying $g$, in the range $\log g$ (cm/s$^2$) = 13.6–15.4] and a set which is constructed with $B$ and $T_{eff}$ varying across the surface according to the magnetic dipole model ($\theta_m$ is the angle between the direction to the observer and the magnetic axis). Effective temperatures span the range $\log T_{eff} (K)$ = 5.5–6.8. Models with single ($B$,$T_{eff}$) cover the energy range 0.05–10 keV, while models with ($B$,$T_{eff}$)-distributions cover the range 0.09–5 keV.

par1 $\log T_{eff}$, surface (unredshifted) effective temperature
par2 $M$, neutron star gravitational mass
par3 $R$, neutron star radius
par4 $d$, distance to neutron star
par5 switch indicating model to use
norm 1, normalization (though not strictly correct, can be varied to change the size of the emission region, ($R_{em}/R)^2$)

The models available by setting par5 are:

Switch Element $B$($10^{12}$ G) $\Theta_B$ $\theta_m$ $\log g$ (cm/s$^2$) $\log T_{eff}$ $E$ (keV)
1000 H 0.01 0 N/A 2.4 5.5 – 6.7 0.05 – 10
1060 H 0.04 0 N/A 0.4 – 2.5 5.5 – 6.7 0.05 – 10
1085 H 0.07 0 N/A 0.4 – 2.5 5.5 – 6.7 0.05 – 10
1100 H 0.1 0 N/A 0.4 – 2.5 5.5 – 6.7 0.05 – 10
1170 H 0.5 0 N/A 0.4 – 2.5 5.5 – 6.8 0.05 – 10
1185 H 0.71 0 N/A 2.4 5.5 – 6.8 0.05 – 10
1195 H 0.89 0 N/A 2.4 5.5 – 6.8 0.05 – 10
1200 H 1.0 0 N/A 0.4 – 2.5 5.5 – 6.8 0.05 – 10
1230 H 2.0 0 N/A 2.4 5.5 – 6.8 0.05 – 10
1260 H 4.0 0 N/A 2.4 5.5 – 6.8 0.05 – 10
1280 H 7.0 0 N/A 2.4 5.5 – 6.8 0.05 – 10
1300 H 10.0 0 N/A 0.4 – 2.5 5.5 – 6.8 0.05 – 10
1330 H 20.0 0 N/A 2.4 5.6 – 6.8 0.05 – 10
1350 H 30.0 0 N/A 2.4 5.7 – 6.8 0.05 – 10
1211 H 1.26 0 N/A 1.6 5.5 – 6.8 0.05 – 10
1281 H 7.0 0 N/A 1.6 5.5 – 6.8 0.05 – 10
12006 C 1.0 0 N/A 2.4 5.8 – 6.9 0.05 – 10
13006 C 10.0 0 N/A 2.4 5.8 – 6.9 0.05 – 10
12008 O 1.0 0 N/A 2.4 5.8 – 6.9 0.05 – 10
13008 O 10.0 0 N/A 2.4 5.8 – 6.9 0.05 – 10
12010 Ne 1.0 0 N/A 2.4 5.8 – 6.9 0.05 – 10
13010 Ne 10.0 0 N/A 2.4 5.8 – 6.9 0.05 – 10
123100 H 1.0 – 1.82 0-90 0 1.6 5.5 – 6.8 0.09 – 5
123190 H 1.0 – 1.82 0-90 90 1.6 5.5 – 6.8 0.09 – 5
130100 H 5.5 – 10.0 0-90 0 1.6 5.5 – 6.8 0.09 – 5
130190 H 5.5 – 10.0 0-90 90 1.6 5.5 – 6.8 0.09 – 5

If you publish results obtained using nsmaxg, please reference Ho (2014).

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Next: nsx: neutron star with Up: Additive Model Components Previous: nsmax: Neutron Star Magnetic   Contents