Spectra From Magnetized, Accreting Neutron Stars: the Proton Cyclotron Feature

Details Spectra From Magnetized, Accreting Neutron Stars: the Proton Cyclotron Feature Spectra From Magnetized, Accreting Neutron Stars: the Proton Cyclotron Feature

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998tx19.confe.260z&link_type=abstract

Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.:

Astronomy and Astrophysics

Astrophysics

Scientific paper

Spectra emitted by strongly magnetized (B 1012 G), accreting neutron stars are computed for different values of the accretion rate, under conditions typical of X-ray sources. The radiation field is derived by solving the transfer equations for the two normal polarization modes in a plane-parallel atmosphere at energies below the electron gyrofrequency. We consider a fully-ionized hydrogen plasma accounting for electron-ion bremsstrahlung, scattering and including the effects of vacuum polarization. As in the non-magnetic case, spectra are harder than the blackbody at the star effective temperature and show a prominent emission feature in the optical-UV band at the proton cyclotron frequency.

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