Statistics – Computation
Scientific paper
Mar 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...338..343w&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 338, March 1, 1989, p. 343-358.
Statistics
Computation
30
Computational Astrophysics, Cyclotron Radiation, Neutron Stars, Stellar Atmospheres, Stellar Mass Accretion, Energy Spectra, Line Spectra, Magnetic Stars, Photons, Radiative Transfer, Relativistic Theory, Stellar Magnetic Fields
Scientific paper
Cyclotron line features from the polar cap plasmas of accreting magnetized neutron stars are modeled. The polar cap environment is modeled by a homogeneous isothermal plane-parallel slab threaded by a uniform superstrong magnetic field oriented orthogonal to the slab. Two physical cyclotron photon source functions are used. For conventional stopping depths, the emergent line spectra are fairly independent of the source functions. For hot atmospheres the details of the line transfer using relativistic kinematics differ substantially from those using nonrelativistic kinematics. Aside from finite recoil, both a finite natural linewidth and conventional stopping depths suppress the escape of photons blueward of line center and potential line features tend to be smeared out into the low-energy continuum. The formation of a line features is most favorable in low-field high-temperature atmospheres where cyclotron photon production is confined to a layer of small column density.
Salpeter Edwin E.
Wang John C. L.
Wasserman Ira M.
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