Models of magnetized neutron star atmospheres
Abstract
We present a new computer code for modeling magnetized neutron star atmospheres in a wide range of magnetic fields (10^{12} - 10^{15} G) and effective temperatures (3 \times 10^5 - 10^7 K). The atmosphere is assumed to consist either of fully ionized electron-ion plasmas or of partially ionized hydrogen. Vacuum resonance and partial mode conversion are taken into account. Any inclination of the magnetic field relative to the stellar surface is allowed. We use modern opacities of fully or partially ionized plasmas in strong magnetic fields and solve the coupled radiative transfer equations for the normal electromagnetic modes in the plasma. Using this code, we study the possibilities to explain the soft X-ray spectra of isolated neutron stars by different atmosphere models. In particular, the outgoing spectrum using the "sandwich" model (thin atmosphere with a hydrogen layer above a helium layer) is constructed. Thin partially ionized hydrogen atmospheres with vacuum polarization are shown to be able to improve our understanding of the observed spectrum of the nearby isolated neutron star RBS 1223 (RX J1308.8+2127).
Keywords
Cite
@article{arxiv.0909.2997,
title = {Models of magnetized neutron star atmospheres},
author = {V. Suleimanov and A. Y. Potekhin and K. Werner},
journal= {arXiv preprint arXiv:0909.2997},
year = {2010}
}
Comments
17 pages, 5 figures, contribution to the session on "Astrophysical Studies of Neutron Stars from Multiwavelengths Observations" at the 37th COSPAR Scientific Assembly (Montreal, July 2008). To appear in Advances in Space Research