2006A&A...457.1003S


Query : 2006A&A...457.1003S

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 - 2023
#notes
1 V* AX Per Sy* 01 36 22.7004366768 +54 15 02.411547480   11.45 10.67 11.04   M3IIIep+A0 285 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 EB* 04 06 55.8351101323 +33 26 47.009585515       7.71   B3Vn 265 0
4 V* SY Mus Sy* 11 32 09.9955543536 -65 25 11.458124364   11.97 10.20     M4 160 0
5 V* RW Hya Sy* 13 34 18.1289607744 -25 22 48.881433972   11.51 10.00     M1/2IIIe 192 0
6 V* T CrB Sy* 15 59 30.1622265912 +25 55 12.613382940   11.516 10.247 9.70   M3IIIe_sh 680 0
7 V* AG Dra Sy* 16 01 41.0120557968 +66 48 10.135056672 11.50 11.06 9.74 8.52   K3IIIep 490 0
8 PN M 2-9 PN 17 05 37.952 -10 08 34.58   12.59 14.7     Be 516 0
9 V* AE Ara Sy* 17 41 04.9182781488 -47 03 27.189284400   12.16 11.63 12.74   M2-5.5+Be 67 1
10 EM* AS 297 Sy* 18 14 34.1920736832 +20 59 21.189578820     11.10     M2pev 141 0
11 V* AR Pav EB* 18 20 27.8820649248 -66 04 42.928979808   11.36 7.40     B1 152 0
12 EM* MWC 603 Sy* 18 22 07.8548979216 +23 27 19.934869104   12.34 11.52     M3ep+O 115 0
13 V* FN Sgr Sy* 18 53 54.7734717504 -18 59 40.659146196           M5IIIe 55 0
14 V* BF Cyg Sy* 19 23 53.5006095432 +29 40 29.177024952   10.52 9.30     Bep+M5III 269 0
15 V* CH Cyg Sy* 19 24 33.0657463320 +50 14 29.095038672 8.14 8.77 7.08   5.345 M7IIIab+Be 754 0
16 V* CI Cyg Sy* 19 50 11.8342618008 +35 41 03.004794996   11.97 9.90     M4.9III 414 0
17 V* PU Vul Sy* 20 21 13.3111130136 +21 34 18.697391652   11.13 10.87 11.697   M3+F2Ib 299 0
18 V* V1329 Cyg Sy* 20 51 01.2321742512 +35 34 54.111458316       13.36   M4IIIe 298 2
19 V* AG Peg Sy* 21 51 01.9739297352 +12 37 32.127939336   9.85 8.69     M3IIIe 500 0
20 V* Z And Sy* 23 33 39.9553225728 +48 49 05.974867308 8.86 9.35 8.00     M2III+B1eq 513 0

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2022.11.28-12:49:51

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