Non-spherical Mass Outflow from RS Ophiuchi During its 2006 Outburst

被引：0
|
作者：
Skopal, A. [1 ]
Pribulla, T. [1 ]
Buil, Ch. [2 ]
Vittone, A. [3 ]
Errico, L. [3 ]
机构：
[1] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia
[2] Castanet Tolosan Obser, F-31320 Castanet Tolosan, France
[3] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy
来源：
RS OPHIUCHI (2006) AND THE RECURRENT NOVA PHENOMENON | 2008年 / 401卷
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中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present results of our modeling of the H alpha line profile during the 2006 outburst of RS Oph. At day 1.38 it was possible to fit the very broad component of the Ha by a bipolar wind model. The model corresponds to a very fast acceleration of the wind particles, and the line luminosity of similar to 2900(d/1.6 kpc)(2) L-circle dot, to a mass-loss rate of similar to (1 - 2) x 10(-4) M(circle dot)yr(-1). During days 10 - 30 the broad component shrank to FWZI similar to 1800 km s(-1). It could be associated with expanding ring and its satellite components at similar to +/- 2 430 km s(-1) with bipolar jets. Later observations made at; clay 57 and 209 indicated a decrease in both the mass-loss rate (similar to 1 x 10(-5) -1 x 10(-6) M(circle dot)yr(-1)) and the wind acceleration. During the quiet, phase, emission bumps observed sporadically in the line wings could reflect clumpy ejections by the central star.
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页码：227 / +
页数：2
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