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Neutron Star Atmospheres

Published online by Cambridge University Press:  12 April 2016

George G. Pavlov  and
V. E. Zavlin
George G. Pavlov
Affiliation:
The Pennsylvania State University, Department of Astronomy & Astrophysics, 525 Davey Lab, University Park, PA 16802, USA
V. E. Zavlin
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik, 85740 Garching, Germany

Abstract

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Properties of the thermal radiation emitted by neutron stars (NSs) are determined by thin plasma layers (atmospheres) at their surfaces. The NS atmospheres are very different from those of usual stars due to the immense gravity and huge magnetic fields. Current models of hydrogen NS atmospheres show that the spectra deviate substantially from blackbody spectra of the same temperatures. Comparison of the model spectra with recent observations of soft X-ray and UV-optical radiation of NSs yields the surface temperatures considerably lower than those obtained from the blackbody fits. This conclusion have important implications for theories of NS cooling and for understanding fundamental properties of the superdense matter in the NS interiors.

Type
Part 9. Population and Neutron Star Properties
Information
International Astronomical Union Colloquium , Volume 177: Pulsar Astronomy - 2000 and Beyond , 2000 , pp. 613 - 618
Copyright
Copyright © Astronomical Society of the Pacific 2000

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