2005A&A...440..995S


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.26CET20:52:07

2005A&A...440..995S - Astronomy and Astrophysics, volume 440, 995-1031 (2005/9-4)

Disentangling the composite continuum of symbiotic binaries. I. S-type systems.

SKOPAL A.

Abstract (from CDS):

We describe a method of disentangling the composite, 0.12-5µm continuum of symbiotic binaries. The observed SED is determined by the IUE/HST archival spectra and flux-points corresponding to the optical UBVRI and infrared JHKLM photometric measurements. The modeled SED is given by superposition of fluxes from the cool giant, hot stellar source and nebula including the effect of the Rayleigh scattering process and considering influence of the iron curtain absorptions. We applied this method to 21 S-type symbiotic stars during quiescence, activity and eclipses. We isolated four main components of radiation and determined their properties. (i) Stellar radiation from the giant corresponds to a unique luminosity class - normal giants. Characteristic luminosities are 1600±200 and 290±30L for red and yellow giants, respectively in our sample of objects. (ii) Hot object radiation during quiescence consists of the nebular and stellar component. The former radiates at a mean electron temperature of 19000K and its amount of emission suggests a mass-loss rate from giants via the wind at {dot}(M)W= a fewx10–7M/yr. Radiation of the latter conforms well with that of a black-body photosphere at a characteristic temperature of 105000K. The corresponding effective radii are a factor of ∼10 larger than those of white dwarfs, which thus precludes observing the accretor's surface. Extreme cases of AX Per and V443 Her, for which the hot star temperature from the fit is not capable of producing the nebular emission, signal a disk-like structure of the hot stellar source even during quiescence. (iii) Hot object radiation during activity consists of three components - the stellar and the low- and high-temperature nebular radiation. The stellar radiation satisfies that of a black-body photosphere at a low characteristic temperature of ∼22000K (we call it the 1st type of outbursts) or at a very high characteristic temperature of ≃165000K (2nd type of outbursts). All the active objects with a high orbital inclination show features of the 1st-type of outbursts (here Z And, AE Ara, CD-43°14304, TX CVn, BF Cyg, CH Cyg, CI Cyg, AR Pav, AX Per), while AGDra represents the 2nd-type. The presence of a two-temperature type of UV spectrum and an enlargement of effective radii of the stellar source by a factor of ∼10 with respect to the quiescent values during the 1st-type of outburst suggest an expansion of an optically thick medium at the orbital plane in the form of a disk. The low-temperature nebula radiates at a mean electron temperature of 14000K and is subject to eclipses, while the high-temperature nebula, which is seen during eclipses as the only component, is characterized by Te>30000K. Radiative and geometric properties of the main sources of radiation allowed us to reconstruct a basic structure of the hot object during the 1st-type of outburst. There is an edge-on disk around the accretor. Its outer flared rim represents a warm pseudophotosphere of the hot stellar source, whose radiation is Rayleigh attenuated and affected by the iron curtain absorptions in the neutral gas concentrated at the orbital plane. The low-temperature nebula is placed just above/below the disk with a concentration at its edge as to be subject to eclipses and to ``see'' well the central ionizing source. High above/below the orbital plane, there is a hot nebular emitting region.

Abstract Copyright:

Journal keyword(s): methods: data analysis - stars: binaries: symbiotic - stars: fundamental parameters - ultraviolet: stars - accretion, accretion disks

Simbad objects: 22

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Number of rows : 22

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* EG And Sy* 00 44 37.1876042586 +40 40 45.703033630 10.54 8.93 7.22     M2.4III 269 0
2 V* AX Per Sy* 01 36 22.6996835649 +54 15 02.411289057   11.45 10.67 11.04   M3IIIep+A0 278 1
3 EM* MWC 560 Sy* 07 25 51.2841922233 -07 44 08.078237799   10.01 9.70 10.60   M4ep+Beq 187 0
4 V* SY Mus Sy* 11 32 09.9958009466 -65 25 11.458645897   11.97 10.20     M4 156 0
5 * 4 Dra SB* 12 30 06.6714652729 +69 12 03.989989948 8.38 6.57 4.95     M3+IIIa 121 0
6 V* TX CVn Sy* 12 44 42.0645704232 +36 45 50.622366015   10.96 10.15 9.79   K0III+B8/9_sh 116 1
7 V* RW Hya Sy* 13 34 18.1290422733 -25 22 48.885732567   11.51 10.00     M1/2IIIe 189 0
8 BD-21 3873 Sy* 14 16 34.2916048270 -21 45 50.037192663   12.060 10.684     K2e 71 0
9 V* T CrB Sy* 15 59 30.1619486506 +25 55 12.607985109   11.516 10.247 9.70   M3IIIe_sh 660 0
10 V* AG Dra Sy* 16 01 41.0125687664 +66 48 10.131181273 11.50 11.06 9.74 8.52   K3IIIep 479 0
11 V* AE Ara Sy* 17 41 04.9192760059 -47 03 27.195993613   12.16 11.63 12.74   M2-5.5+Be 67 1
12 EM* AS 297 Sy* 18 14 34.1920433871 +20 59 21.188200993     11.10     M2pev 136 0
13 V* AR Pav Al* 18 20 27.8818737427 -66 04 42.931712420   11.36 7.40     B1 146 0
14 EM* MWC 603 Sy* 18 22 07.8547728418 +23 27 19.933241936   12.34 11.52     M3ep+O 114 0
15 V* BF Cyg Sy* 19 23 53.5009795759 +29 40 29.173306238   10.52 9.30     Bep+M5III 269 0
16 V* CH Cyg Sy* 19 24 33.0697620341 +50 14 29.057625755 8.14 8.77 7.08   5.345 M7IIIab+Be 744 0
17 V* CI Cyg Al* 19 50 11.8344401438 +35 41 03.000692799   11.97 9.90     Bep+M5III 410 0
18 V* LT Del Sy* 20 35 57.2353984617 +20 11 27.504214453           G6III 97 1
19 V* V1329 Cyg Sy* 20 51 01.2322054447 +35 34 54.111427235           M4IIIe 296 2
20 CD-43 14304 Sy* 21 00 06.3577224043 -42 38 44.938778022     11.0     K7e 54 0
21 V* AG Peg Sy* 21 51 01.9733955799 +12 37 32.124041390   6.76 6.00     M3IIIe 494 0
22 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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