KFU. Card publication. A Reflection Model for the Cyclotron Lines in the Spectra of X-Ray Pulsars

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A REFLECTION MODEL FOR THE CYCLOTRON LINES IN THE SPECTRA OF X-RAY PULSARS

Form of presentation

Articles in international journals and collections

Year of publication

2013

Authors, employees of KFU

Suleymanov Valeriy Fialovich, author

Bibliographic description in the original language

A Reflection Model for the Cyclotron Lines in the Spectra of X-Ray Pulsars. Poutanen, Juri; Mushtukov, Alexander A.; Suleimanov, Valery F.; Tsygankov, Sergey S.; Nagirner, Dmitrij I.; Doroshenko, Victor; Lutovinov, Alexander A. The Astrophysical Journal, Volume 777, Issue 2, article id. 115, 8 pp. (2013).

Annotation

ASTROPHYS J

Keywords

line: formation, pulsars: general, relativistic processes, scattering, stars: neutron, X-rays: binaries

The name of the journal

ASTROPHYS J

URL

http://ads.ari.uni-heidelberg.de/abs/2013ApJ...777..115P

Please use this ID to quote from or refer to the card

https://repository.kpfu.ru/eng/?p_id=73901&p_lang=2

Full metadata record

Field DC	Value	Language
dc.contributor.author	Suleymanov Valeriy Fialovich	ru_RU
dc.date.accessioned	2013-01-01T00:00:00Z	ru_RU
dc.date.available	2013-01-01T00:00:00Z	ru_RU
dc.date.issued	2013	ru_RU
dc.identifier.citation	A Reflection Model for the Cyclotron Lines in the Spectra of X-Ray Pulsars. Poutanen, Juri; Mushtukov, Alexander A.; Suleimanov, Valery F.; Tsygankov, Sergey S.; Nagirner, Dmitrij I.; Doroshenko, Victor; Lutovinov, Alexander A. The Astrophysical Journal, Volume 777, Issue 2, article id. 115, 8 pp. (2013).	ru_RU
dc.identifier.uri	https://repository.kpfu.ru/eng/?p_id=73901&p_lang=2	ru_RU
dc.description.abstract	ASTROPHYS J	ru_RU
dc.description.abstract	ASTROPHYS J	ru_RU
dc.description.abstract	Cyclotron resonance scattering features observed in the spectra of some X-ray pulsars show significant changes of the line energy with the pulsar luminosity. At high luminosities, these variations are often associated with the onset and growth of the accretion column, which is believed to be the origin of the observed emission and of the cyclotron lines. However, this scenario inevitably implies a large gradient of the magnetic field strength within the line-forming region, which makes the formation of the observed line-like features problematic. Moreover, the observed variation of the cyclotron line energy is much smaller than could be anticipated for the corresponding luminosity changes. We argue here that a more physically realistic situation is that the cyclotron line forms when the radiation emitted by the accretion column is reflected from the neutron star surface, where the gradient of the magnetic field strength is significantly smaller. Here we develop a reflection model and apply it to explain the observed variations of the cyclotron line energy in a bright X-ray pulsar V 0332+53 over a wide range of luminosities.	ru_RU
dc.language.iso	ru	ru_RU
dc.subject	line: formation	ru_RU
dc.subject	pulsars: general	ru_RU
dc.subject	relativistic processes	ru_RU
dc.subject	scattering	ru_RU
dc.subject	stars: neutron	ru_RU
dc.subject	X-rays: binaries	ru_RU
dc.title	A Reflection Model for the Cyclotron Lines in the Spectra of X-Ray Pulsars	ru_RU
dc.type	Articles in international journals and collections	ru_RU