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Article overview
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A non-spherical mass outflow from RS Oph during its 2006 outburst | A. Skopal
; T. Pribulla
; Ch. Buil
; A. Vittone
; L. Errico
; | Date: |
25 Feb 2008 | Abstract: | 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. | Source: | arXiv, 0802.3711 | Services: | Forum | Review | PDF | Favorites |
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