dc.contributor.author | BALMAN, Şölen | |
dc.contributor.author | Ogelman, H | |
dc.contributor.author | Krautter, J | |
dc.date.accessioned | 2021-03-05T10:45:59Z | |
dc.date.available | 2021-03-05T10:45:59Z | |
dc.date.issued | 1998 | |
dc.identifier.citation | BALMAN Ş., Krautter J., Ogelman H., "The X-ray spectral evolution of classical Nova V1974 Cygni 1992: A reanalysis of the ROSAT data", ASTROPHYSICAL JOURNAL, cilt.499, ss.395-406, 1998 | |
dc.identifier.issn | 0004-637X | |
dc.identifier.other | vv_1032021 | |
dc.identifier.other | av_a4d11b3d-7ae2-4b86-84df-c0a0873ba73d | |
dc.identifier.uri | http://hdl.handle.net/20.500.12627/110239 | |
dc.identifier.uri | https://doi.org/10.1086/305600 | |
dc.description.abstract | We present a spectral analysis of the archival X-ray data of classical Nova V1974 Cygni 1992 (Nova Cygni 1992) obtained by the ROSAT Position Sensitive Proportional Counter (PSPC). The X-ray spectrum is fitted with a two-component model. The first component is a white dwarf atmosphere emission model developed for the remnants of classical novae near the Eddington luminosity. The model is used to fit the soft X-ray data in the similar to 0.1-1.0 keV range, where the bulk of emission is below 0.7 keV. The second component is a Raymond-Smith model of thermal plasma applied to the hard X-ray emission above similar to 1.0 keV. The postoutburst X-ray spectrum of the remnant white dwarf is examined in the context of evolution on the Hertzsprung-Russell diagram using an O-Ne- and a C-O-enhanced atmosphere emission model. A constant bolometric luminosity evolution is detected with increasing effective temperature and decreasing photospheric radius using the O-Ne-enhanced model. The unabsorbed soft X-ray flux for the constant bolometric luminosity phase is found to be in the range (1.7-2.2) x 10(-7) ergs s(-1) cm(-2). A peak effective temperature of 51 eV (5.9 x 10(5) K) is detected 511 days after outburst. We also present the spectral development of the hard X-ray component. It is found to evolve independently of the soft one. The maximum of the hard X-ray emission is reached at similar to 150 days after outburst with an unabsorbed flux of similar to 2.0 x 10(-11) ergs s(-1) cm(-2) corresponding to a luminosity of (0.8-2.0)x 10(34) ergs s(-1) at a 2-3 kpc source distance. The time evolution of the hard X-ray flux and the plasma temperatures decreasing from 10 keV to 1 keV suggest emission from shock-heated gas as the origin of the hard X-ray component. | |
dc.language.iso | eng | |
dc.subject | Uzay bilimi | |
dc.subject | Temel Bilimler | |
dc.subject | ASTRONOMİ VE ASTROFİZİK | |
dc.subject | Astronomi ve Astrofizik | |
dc.subject | Fizik | |
dc.subject | Temel Bilimler (SCI) | |
dc.title | The X-ray spectral evolution of classical Nova V1974 Cygni 1992: A reanalysis of the ROSAT data | |
dc.type | Makale | |
dc.relation.journal | ASTROPHYSICAL JOURNAL | |
dc.contributor.department | , , | |
dc.identifier.volume | 499 | |
dc.identifier.issue | 1 | |
dc.identifier.startpage | 395 | |
dc.identifier.endpage | 406 | |
dc.contributor.firstauthorID | 2212678 | |