Issue |
A&A
Volume 433, Number 1, April I 2005
|
|
---|---|---|
Page(s) | 275 - 283 | |
Section | Stellar structure and evolution | |
DOI | https://doi.org/10.1051/0004-6361:20041612 | |
Published online | 14 March 2005 |
Thermal radiation from magnetic neutron star surfaces
Departament de Física Aplicada, Universitat d'Alacant, Ap. Correus 99, 03080 Alacant, Spain
Received:
7
July
2004
Accepted:
22
November
2004
We investigate the thermal emission from magnetic neutron star surfaces
in which the cohesive effects of the magnetic field have produced the condensation
of the atmosphere and the external layers. This may happen for sufficiently
cool () atmospheres with moderately intense magnetic fields
(about 1013 G for Fe atmospheres). The thermal emission from an isothermal
bare surface of a neutron star shows no remarkable spectral features, but
it is significantly depressed at energies below some threshold energy. However, since the thermal
conductivity is very different in the normal and parallel directions to the magnetic
field lines, the presence of the magnetic field is expected to produce a highly anisotropic
temperature distribution, depending on the magnetic field geometry. In this case
the observed flux of such an object looks very similar to a BB spectrum, but depressed
by a nearly constant factor at all energies. This results in a systematic
underestimation of the area of the emitter (and therefore its size) by a factor 5–10 (2–3).
Key words: stars: neutron / radiation mechanisms: thermal / X-rays: stars
© ESO, 2005
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