RS Ophiuchi in Quiescence: Why is it X-ray Faint?
| dc.creator | Mukai, Koji | |
| dc.date | 2008-03-19 | |
| dc.date.accessioned | 2026-07-07T09:27:37Z | |
| dc.date.available | 2026-07-07T09:27:37Z | |
| dc.description | The short interval between successive outbursts of RS Oph strongly suggests that it has a high mass white dwarf accreting at a high rate. This, in turn, suggests the possibility of prominent X-ray emission from RS Oph in quiescence. However, archival quiescent X-ray observations of RS Oph show it to be a modest soft X-ray source but not a strong 2-10 keV X-ray source. In this aspect, RS Oph differs markedly from T CrB. We speculate on the possible mechanisms that could significantly suppress the 2-10 keV X-ray emission in RS Oph. | |
| dc.description | 4 pages, 1 figure, RS Oph (2006), Keele, UK, conference proceeding | |
| dc.identifier | https://arxiv.org/abs/0803.2912 | |
| dc.identifier | http://arxiv.org/abs/0803.2912 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/157166 | |
| dc.subject | Astrophysics | |
| dc.title | RS Ophiuchi in Quiescence: Why is it X-ray Faint? | |
| dc.type | text |