2006A&A...457.1003S


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.03CET04:20:42

2006A&A...457.1003S - Astronomy and Astrophysics, volume 457, 1003-1010 (2006/10-3)

Broad Hα wings from the optically thin stellar wind of the hot components in symbiotic binaries.

SKOPAL A.

Abstract (from CDS):

To model broad Hα wings observed in symbiotic binaries by an optically thin, bipolar stellar wind from their hot components as an alternative to that considering the Raman scattering of Lyβ photons on atomic hydrogen. Profile-fitting analysis. Comparison of the observed broad Hα wings and their luminosity with those predicted by the model. Synthetic Hα profiles fit excellently the observed wings for |Δv|>200km/s in our sample of 10 symbiotic stars during the quiescent as well as active phases. The wing profile formed in the stellar wind can be approximated by a function f(Δv)∝Δv–2, which is of the same type as that arising from the Raman scattering. Therefore it is not possible to distinguish between these two processes only by modeling the line profile. Some observational characteristics of the Hα-emission, its relationship with the emission measure of the symbiotic nebula and a steep radio spectrum at 1.4-15GHz suggest the ionized stellar wind from the hot component to be the dominant source contributing to the Hα wings during active phases. The model corresponding mass-loss rates from the hot components are of a fewx10–8M/yr and of a fewx(10–7-10–6)M/yr during quiescent and active phases, respectively.

Abstract Copyright:

Journal keyword(s): stars: binaries: symbiotics - stars: mass-loss - stars: winds, outflows

Simbad objects: 20

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Number of rows : 20

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 V* AX Per Sy* 01 36 22.6996835649 +54 15 02.411289057   11.45 10.67 11.04   M3IIIep+A0 278 1
2 V* AG Per A SB* 04 06 55.828400 +33 26 46.92224   6.83 6.87     ~ 255 0
3 V* AG Per Al* 04 06 55.8351101323 +33 26 47.009585515       7.71   B3Vn 262 0
4 V* SY Mus Sy* 11 32 09.9958009466 -65 25 11.458645897   11.97 10.20     M4 156 0
5 V* RW Hya Sy* 13 34 18.1290422733 -25 22 48.885732567   11.51 10.00     M1/2IIIe 189 0
6 V* T CrB Sy* 15 59 30.1619486506 +25 55 12.607985109   11.516 10.247 9.70   M3IIIe_sh 661 0
7 V* AG Dra Sy* 16 01 41.0125687664 +66 48 10.131181273 11.50 11.06 9.74 8.52   K3IIIep 479 0
8 PN M 2-9 PN 17 05 37.952 -10 08 34.58   12.59 14.7     Be 507 0
9 V* AE Ara Sy* 17 41 04.9192760059 -47 03 27.195993613   12.16 11.63 12.74   M2-5.5+Be 67 1
10 EM* AS 297 Sy* 18 14 34.1920433871 +20 59 21.188200993     11.10     M2pev 136 0
11 V* AR Pav Al* 18 20 27.8818737427 -66 04 42.931712420   11.36 7.40     B1 146 0
12 EM* MWC 603 Sy* 18 22 07.8547728418 +23 27 19.933241936   12.34 11.52     M3ep+O 114 0
13 V* FN Sgr Sy* 18 53 54.7732843778 -18 59 40.660080929           M5IIIe 52 0
14 V* BF Cyg Sy* 19 23 53.5009795759 +29 40 29.173306238   10.52 9.30     Bep+M5III 269 0
15 V* CH Cyg Sy* 19 24 33.0697620341 +50 14 29.057625755 8.14 8.77 7.08   5.345 M7IIIab+Be 745 0
16 V* CI Cyg Al* 19 50 11.8344401438 +35 41 03.000692799   11.97 9.90     Bep+M5III 410 0
17 V* PU Vul No* 20 21 13.3112218215 +21 34 18.693825946   11.13 10.87     A4II-F8Iab+M6IIIe 297 0
18 V* V1329 Cyg Sy* 20 51 01.2322054447 +35 34 54.111427235           M4IIIe 296 2
19 V* AG Peg Sy* 21 51 01.9733955799 +12 37 32.124041390   6.76 6.00     M3IIIe 494 0
20 V* Z And Sy* 23 33 39.9551345051 +48 49 05.973842875 8.86 9.35 8.00     M2III+B1eq 505 0

    Equat.    Gal    SGal    Ecl

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2021.03.03-04:20:42

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