2015A&A...577A..55D


C.D.S. - SIMBAD4 rel 1.7 - 2020.09.19CEST05:11:32

2015A&A...577A..55D - Astronomy and Astrophysics, volume 577A, 55-55 (2015/5-1)

Non-conservative evolution in Algols: where is the matter?

DESCHAMPS R., BRAUN K., JORISSEN A., SIESS L., BAES M. and CAMPS P.

Abstract (from CDS):

There is indirect evidence of non-conservative evolutions in Algols. However, the systemic mass-loss rate is poorly constrained by observations and generally set as a free parameter in binary-star evolution simulations. Moreover, systemic mass loss may lead to observational signatures that still need to be found. Within the ''hotspot'' ejection mechanism, some of the material that is initially transferred from the companion star via an accretion stream is expelled from the system due to the radiative energy released on the gainer's surface by the impacting material. The objective of this paper is to retrieve observable quantities from this process and to compare them with observations. We investigate the impact of the outflowing gas and the possible presence of dust grains on the spectral energy distribution (SED). We used the 1D plasma code Cloudy and compared the results with the 3D Monte-Carlo radiative transfer code Skirt for dusty simulations. The circumbinary mass-distribution and binary parameters were computed with state-of-the-art binary calculations done with the Binstar evolution code.The outflowing material reduces the continuum flux level of the stellar SED in the optical and UV. Because of the time-dependence of this effect, it may help to distinguish between different ejection mechanisms. If present, dust leads to observable infrared excesses, even with low dust-to-gas ratios, and traces the cold material at large distances from the star. By searching for this dust emission in the WISE catalogue, we found a small number of Algols showing infrared excesses, among which the two rather surprising objects SX Aur and CZ Vel. We find that some binary B[e] stars show the same strong Balmer continuum as we predict with our models. However, direct evidence of systemic mass loss is probably not observable in genuine Algols, since these systems no longer eject mass through the hotspot mechanism. Furthermore, owing to its high velocity, the outflowing material dissipates in a few hundred years. If hot enough, the hotspot may produce highly ionised species, such as SiIV, and observable characteristics that are typical of W Ser systems. If present, systemic mass loss leads to clear observational imprints. These signatures are not to be found in genuine Algols but in the closely related β Lyraes, W Serpentis stars, double periodic variables, symbiotic Algols, and binary B[e] stars. We emphasise the need for further observations of such objects where systemic mass loss is most likely to occur.

Abstract Copyright:

Journal keyword(s): binaries: general - radiative transfer - circumstellar matter - methods: numerical

Simbad objects: 34

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Number of rows : 34

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9510 1
2 * phi Per Be* 01 43 39.6379209 +50 41 19.432832 3.10 4.02 4.06 3.90 3.88 B1.5V:e-shell 532 0
3 V* RX Cas bL* 03 07 45.7481570255 +67 34 38.614798549   10.14 8.64     K1III+A5eIII 173 0
4 * bet Per Al* 03 08 10.1324535 +40 57 20.328013 1.70 2.07 2.12 2.08 2.11 B8V 1150 2
5 V* AS Eri Al* 03 32 25.1262238528 -03 18 48.096045754   8.49 8.30     A1V 159 0
6 HD 33357 Be* 05 11 42.9273627502 +42 09 55.278557789 7.67 8.55 8.55     B1:V:ne 171 0
7 V* V617 Aur bL* 05 39 56.62399 +30 05 11.2366   8.86 8.15     F4III 37 1
8 HD 41335 Be* 06 04 13.5022124890 -06 42 32.225555101 4.31 5.14 5.21 5.13 5.09 B3/5Vnne 274 0
9 * 17 Lep Sy* 06 04 59.1294088750 -16 29 03.968723282 5.29 5.17 4.93     A3+K/M 196 0
10 NAME Mon R2 HII 06 07 46.6 -06 22 59           ~ 654 2
11 HD 43246 SB* 06 16 22.1983433965 +28 51 07.132404490   7.82 7.41     A0Vn+F5III 42 0
12 HD 45910 Be* 06 30 32.9372530321 +05 52 01.205747083 6.64 7.18 6.85 6.31 5.81 B2IIIe 214 0
13 V* V509 Mon Al* 06 47 10.7214269836 -01 02 14.736534090     14.42     G4IV 10 0
14 HD 50846 Al* 06 54 54.7083961175 -01 22 32.849416553   8.46 8.43     B5/7Ib 134 0
15 HD 51480 Be* 06 57 09.3837228593 -10 49 28.062219265 6.66 7.24 6.93 7.78   Be_sh 85 0
16 V* UX Mon Al* 07 59 16.3751282592 -07 30 17.889948033   8.74 8.42     A2/3+G/K 124 0
17 V* DM Pup Al* 08 07 04.0940130969 -25 31 52.244515656           A2.5 6 0
18 V* CZ Vel Al* 09 10 44.4646673848 -50 42 40.606198596   11.57 10.80     B6 9 0
19 V* W Cru bL* 12 11 59.1618206802 -58 47 00.737393202   9.47 8.44     F8/G1Ia/abe 90 0
20 V* U CrB Al* 15 18 11.3525714546 +31 38 49.412035589   7.79 7.83     B6V 248 0
21 V* UZ Nor Al* 16 28 11.5594675594 -53 19 21.646818213 11.09 11.34 11.29     B 9 0
22 V* W Ser Al* 18 09 50.6487890730 -15 33 00.269169421   9.64 8.42     F8/G2Iaep(+A) 128 0
23 V* RY Sct Be* 18 25 31.4772031860 -12 41 24.196044092 10.25 10.38 9.12 9.46   O9.7Ibep 284 1
24 V* RZ Sct Al* 18 26 33.5234774335 -09 12 05.988849324 8.09 8.24 7.53     B2/3Ib/II 160 0
25 V* V930 Oph Al* 18 41 45.6496763709 +12 02 11.114459745           ~ 6 0
26 HD 174237 Be* 18 46 43.0889592280 +52 59 16.650319177 5.06 5.80 5.90     B3+F5III 191 0
27 V* DH Her Al* 18 47 34.5584722582 +22 50 45.795930647   10.55 10.50     A5 24 0
28 V* V356 Sgr Al* 18 47 52.3313273686 -20 16 28.244431656   7.07 6.99     B9III 163 0
29 * bet Lyr bL* 18 50 04.7952472 +33 21 45.609978 2.85 3.42 3.42 3.31 3.29 B8.5Ib-II 886 0
30 V* V367 Cyg bL* 20 47 59.5848515369 +39 17 15.722701131 8.080 7.680 6.990     A3Ibep 197 0
31 HD 207739 SB* 21 49 58.8415737575 +43 57 56.833556720   9.22 8.59     kF0:mGepec 62 0
32 * pi. Aqr Be* 22 25 16.6228499 +01 22 38.634579 3.64 4.60 4.64 4.48 4.48 B1III-IVe 385 0
33 HD 218393 Be* 23 07 06.2120465053 +50 11 32.489137162 6.79 7.25 6.92     B3pe+K1III 145 0
34 V* V442 Cas Al* 23 40 14.7999084781 +53 57 33.990611529   13.06 12.74     M5V 18 0

    Equat.    Gal    SGal    Ecl

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2020.09.19-05:11:32

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