A non-spherical mass outflow from RS Oph during its 2006 outburst
| dc.creator | Skopal, A. | |
| dc.creator | Pribulla, T. | |
| dc.creator | Buil, Ch. | |
| dc.creator | Vittone, A. | |
| dc.creator | Errico, L. | |
| dc.date | 2008-02-25 | |
| dc.date.accessioned | 2026-07-07T09:23:15Z | |
| dc.date.available | 2026-07-07T09:23:15Z | |
| dc.description | We present results of our modeling the H-alpha line profile along the 2006 RS Oph outburst. At day 1.38 the very broad component of the H-alpha profile was possible to fit by a bipolar wind model. The model corresponds to a very fast acceleration of the wind particles, and the line luminosity of about 2900 (d/1.6 kpc)^2 solar luminosities to the mass-loss rate of around (1-2) x 10E-4 solar masses per year. During days 10-30 the broad component shrank to FWZI = 1800 km/s. It could be associated with expanding ring and its satellite components at about +/- 2430 km/s with bipolar jets. Later observations made at day 57 and 209 indicated a decrease in both the mass-loss rate (1xE-5 - 1xE-6 solar masses per year) and the wind acceleration. During the quiet phase, emission bumps observed sporadically in the line wings could reflect clumpy ejections by the central star. | |
| dc.description | 4 pages, 3 figures, will appear in the proceedings of the conference, RS Ophiuchi (2006) | |
| dc.identifier | https://arxiv.org/abs/0802.3711 | |
| dc.identifier | http://arxiv.org/abs/0802.3711 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/155666 | |
| dc.subject | Astrophysics | |
| dc.title | A non-spherical mass outflow from RS Oph during its 2006 outburst | |
| dc.type | text |