Zobrazeno 91 - 100
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pro vyhledávání: '"A, Gvaramadze"'
Autor:
Gvaramadze, V. V.
Publikováno v:
A&A, 2001, v. 374, pp. 259-263
It is generally accepted that the PSR B1509-58 is associated with the supernova remnant (SNR) MSH 15-52 (G 320.4-01.2). The spin-down age of the pulsar is \simeq 1700 years, while the size and the general appearance of the SNR suggest that this syste
Externí odkaz:
http://arxiv.org/abs/astro-ph/0102431
Autor:
Gvaramadze, Vasilii
Publikováno v:
A&A, 2001, v.369, pp.174-177
It is shown that if the shell of the Vela supernova remnant is responsible for nearly all the scattering of the Vela pulsar, then the scintillation and proper motion velocities of the pulsar can only be reconciled with each other in the case of nonze
Externí odkaz:
http://arxiv.org/abs/astro-ph/0005580
Autor:
Gvaramadze, V. V.
It is pointed out that a cavity supernova (SN) explosion of a moving massive star could result in a significant offset of the neutron star (NS) birth-place from the geometrical centre of the supernova remnant (SNR). Therefore: a) the high implied tra
Externí odkaz:
http://arxiv.org/abs/astro-ph/0005572
Autor:
Gvaramadze, V. V.
Publikováno v:
Odessa Astron. Publ., 12 (1999) 117
Most of middle-aged supernova remnants (SNRs) have a distorted and complicated appearance which cannot be explained in the framework of the Sedov-Taylor model. We consider three typical examples of such SNRs (Vela SNR, MSH 15-52, G 309.2-00.6) and sh
Externí odkaz:
http://arxiv.org/abs/astro-ph/9912512
Autor:
Gvaramadze, V. V.
Publikováno v:
Astron. Astrophys., 352 (1999) 712
The nature of the Vela X-ray "jet", recently discovered by Markwardt & \"Ogelman (1995), is examined. It is suggested that the "jet" arises along the interface of domelike deformations of the Rayleigh-Taylor unstable shell of the Vela supernova remna
Externí odkaz:
http://arxiv.org/abs/astro-ph/9912049
Autor:
V. V. Gvaramadze
Publikováno v:
Odessa Astronomical Publications, Vol 12, Iss 0, Pp 117-120 (2017)
Most of middle-aged supernova remnants (SNRs) have a distorted and complicated appearance which cannot be explained in the framework of the Sedov-Taylor model. We consider three typical examples of such SNRs (Vela SNR, MSH15-52, G309.2-00.6) and show
Externí odkaz:
https://doaj.org/article/41ff5c547d8d4d4193b9d993a2a6b6be
Publikováno v:
Monthly Notices of the Royal Astronomical Society
Luminous blue variables (LBVs) are massive stars that show strong spectral and photometric variability. The questions of what evolutionary stages they represent and what exactly drives their instability are still open, and thus it is important to und
Akademický článek
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Akademický článek
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Autor:
Mackey, Jonathan, Green, Samuel, Haworth, Thomas, Kavanagh, Patrick, Moutzouri, Maria, Gvaramadze, Vasilii V.
Hot massive stars have strong stellar winds with velocity 1000-3000 km/s that, when shocked, produce hot gas with temperature 107−108 K. This is observed as diffuse X-ray emission in Wolf-Rayet nebulae, around young star clusters, and around the ne
Externí odkaz:
https://explore.openaire.eu/search/publication?articleId=doi_dedup___::a33cca705a38764b6b7d6c8ef97b459d