2010MNRAS.407..734M


Query : 2010MNRAS.407..734M

2010MNRAS.407..734M - Mon. Not. R. Astron. Soc., 407, 734-748 (2010/September-2)

High-dispersion spectroscopy of two a supergiant systems in the small Magellanic cloud with novel properties.

MENNICKENT R.E. and SMITH M.A.

Abstract (from CDS):

We present the results of a spectroscopic investigation of two novel variable bright blue stars in the SMC, OGLE004336.91-732637.7 (SMC-SC3) and the periodically occulted star OGLE004633.76-731204.3 (SMC-SC4), whose photometric properties were reported by Mennickent et al. (2010). High-resolution spectra in the optical and far-UV show that both objects are actually A + B type binaries. Three spectra of SMC-SC4 show radial velocity variations, consistent with the photometric period of 184.26 d found in Mennickent et al. 2010. The optical spectra of the metallic lines in both systems show combined absorption and emission components that imply that they are formed in a flattened envelope. A comparison of the radial velocity variations in SMC-SC4 and the separation of the V and R emission components in the Hα emission profile indicate that this envelope, and probably also the envelope around SMC-SC3, is a circumbinary disc with a characteristic orbital radius some three times the radius of the binary system. The optical spectra of SMC-SC3 and SMC-SC4 show, respectively, Hei emission lines and discrete blue absorption components (BACs) in metallic lines. The high excitations of the Hei lines in the SMC-SC3 spectrum and the complicated variations of Feii emission and absorption components with orbital phase in the spectrum of SMC-SC4 suggests that shocks occur between the winds and various static regions of the stars' corotating binary-disc complexes. We suggest that BACs arise from wind shocks from the A star impacting the circumbinary disc and a stream of former wind-efflux from the B star accreting on to the A star. The latter picture is broadly similar to mass transfer occurring in the more evolved (but less massive) algol (B/A + K) systems, except that we envision transfer occurring in the other direction and not through the inner Lagrangian point. Accordingly, we dub these objects prototype of a small group of Magellanic Cloud wind-interacting A + B binaries.

Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS

Journal keyword(s): stars: early-type - stars: evolution - stars: mass-loss - stars: winds, outflows

Simbad objects: 19

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Number of rows : 19
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 LHA 115-S 3 Em* 00 43 36.8879622984 -73 26 38.221533492 14.26 14.39 14.09   13.73 A7-F5Ie 14 0
2 LIN 81 EB* 00 46 33.7454642856 -73 12 04.701631392 14.18 14.21 13.95   13.62 F5Ie+G0I 14 0
3 LIN 166 Em* 00 51 00.1838555160 -72 53 04.262775468 12.55 13.55 13.56   13.52 B1II-IIIe 28 0
4 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10367 1
5 SV* HV 1620 EB* 00 54 38.2336666176 -72 32 06.414177876 13.36 14.34 14.45 14.62 14.68 B0.5(IV)e? 33 0
6 [MA93] 836 Em* 00 55 20.2840702776 -72 37 10.350714612 14.51 14.91 14.84   14.44 A0Ibe 10 0
7 Cl* NGC 330 ARP 3 * 00 56 09.4059802800 -72 27 58.864347972 13.33 14.09 14.22 14.568 14.36 B1II 29 0
8 NGC 330 Cl* 00 56 20.59 -72 27 12.5 9.37 9.76 9.55   8.89 ~ 389 0
9 AzV 194 Be? 00 57 45.2673414408 -72 35 32.558993844 12.66 13.677 13.823   13.94 B1III 12 0
10 LIN 495 Em* 01 12 19.7039927664 -73 51 26.026075188 14.62 14.61 14.63   14.49 (kA5mF0)/B[e] 19 0
11 SV* HV 915 RV* 05 14 18.1109835264 -69 12 34.872203808 15.837 14.924 14.552 13.96 13.853 F7-9Ibpe 26 0
12 [BE74] 561 EB* 05 19 47.7007510680 -69 39 12.161158776   13.76 13.56 13.95 13.461 F6 12 0
13 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16252 1
14 HD 37367 * 05 39 18.3135535104 +29 12 54.788852916 5.6 6.116 5.984     B2IV-V 127 0
15 HD 45057 * 06 22 18.8326760688 -53 20 05.396114364 6.16 6.728 6.855     B3V 22 0
16 HD 45047 * 06 25 41.0460216552 +11 13 12.025014780   7.98 6.77     K0 3 0
17 * n Vel * 08 41 13.1290014504 -47 19 01.669533384 5.01 4.89 4.77 4.56 4.37 A5II 49 0
18 * y Car sg* 11 12 36.0132333384 -60 19 03.454684572 5.20 5.17 4.62 4.07 3.71 A5Iae: 91 0
19 HD 201836 Be* 21 10 30.95640 +47 41 32.0176 6.1         B6IV 56 0

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2022.09.28-03:10:34

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