2013A&A...560A..10C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST04:26:08

2013A&A...560A..10C - Astronomy and Astrophysics, volume 560A, 10-10 (2013/12-1)

The supergiant B[e] star LHA 115-S 18 - binary and/or luminous blue variable?

CLARK J.S., BARTLETT E.S., COE M.J., DORDA R., HABERL F., LAMB J.B., NEGUERUELA I. and UDALSKI A.

Abstract (from CDS):

The mechanism by which supergiant (sg)B[e] stars support cool, dense dusty discs/tori and their physical relationship with other evolved, massive stars such as luminous blue variables is uncertain. In order to investigate both issues we have analysed the long term behaviour of the canonical sgB[e] star LHA 115-S 18. We employed the OGLE II-IV lightcurve to search for (a-)periodic variability and supplemented these data with new and historic spectroscopy. In contrast to historical expectations for sgB[e] stars, S18 is both photometrically and spectroscopically highly variable. The lightcurve is characterised by rapid aperiodic ``flaring'' throughout the 16 years of observations. Changes in the high excitation emission line component of the spectrum imply evolution in the stellar temperature - as expected for luminous blue variables - although somewhat surprisingly, spectroscopic and photometric variability appears not to be correlated. Characterised by emission in low excitation metallic species, the cool circumstellar torus appears largely unaffected by this behaviour. Finally, in conjunction with intense, highly variable Heii emission, X-ray emission implies the presence of an unseen binary companion. S18 provides observational support for the putative physical association of (a subset of) sgB[e] stars and luminous blue variables. Given the nature of the circumstellar environment of S18 and that luminous blue variables have been suggested as supernovae progenitors, it is tempting to draw a parallel to the progenitors of SN1987A and SN2009ip. Moreover the likely binary nature of S18 strengthens the possibility that the dusty discs/tori that characterise sgB[e] stars are the result of binary-driven mass-loss; consequently such stars may provide a window on the short lived phase of mass-transfer in massive compact binaries.

Abstract Copyright:

Journal keyword(s): binaries: close - stars: early-type - stars: emission-line, Be - stars: massive

CDS comments: Footnote 7 : J013459.47+303424.7 is a misprint for LGGS J013459.47+303701.9 or LGGS J013426.11+303424.7

Simbad objects: 35

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Number of rows : 35

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 LHA 115-S 6 s*b 00 46 55.0295095056 -73 08 34.139503944 12.14 13.02 12.91   12.52 B0/0.5[e] 77 1
2 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9440 1
3 LHA 115-S 18 Em* 00 54 09.5415603586 -72 41 43.291670748 12.94 13.48 13.82   12.55 B[e] 76 0
4 HD 5980 WR* 00 59 26.5847969465 -72 09 53.927725716   11.13 11.31   11.029 WN4+O7I: 359 1
5 LGGS J013327.26+303909.3 WR* 01 33 27.2192432287 +30 39 09.070547320 16.750 17.786 17.954 17.906 17.889 Ofpe/WN9 12 0
6 M 33 GiG 01 33 50.904 +30 39 35.79 6.17 6.27 5.72     ~ 5134 1
7 [MCM2000] Em 50 s*b 01 34 26.0853357851 +30 34 24.566359349 18.38 19.23 18.97 18.59 18.27 cLBV 11 0
8 GALEX 2482576446735777935 s*b 01 34 59.4431989969 +30 37 01.718171618 17.35 18.59 18.37 17.88 17.69 cLBV 11 0
9 NAME Romano's Star WR* 01 35 09.7011265200 +30 41 57.173367187   16.5 18.04     Ofpe/WN9 45 1
10 CPD-75 116 s*b 01 44 03.8712992159 -74 40 49.801190680   11.54 11.43 11.69   B5Ia[e] 76 0
11 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5665 1
12 V* CI Cam HXB 04 19 42.1353986687 +55 59 57.708146070 12.13 12.41 11.77 10.79 9.99 B0/2I[e] 224 0
13 HD 34664 s*b 05 13 52.9943883589 -67 26 54.822130587 11.509 11.88 11.774 11.63 10.991 B0/0.5I[e] 94 0
14 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4484 2
15 HD 37974 s*b 05 36 25.8537892343 -69 22 55.789283933 10.056 11.12 10.99 11.00 10.423 B0.5e 114 0
16 W61 7-27 s*b 05 38 57.3147296670 -69 07 09.775903205 14.514 13.891 14.134 13.98 12.884 B3Ia 19 0
17 HD 38489 s*b 05 40 13.3208554964 -69 22 46.485104413 11.236 12.295 11.93 11.79 10.891 B[e] 81 1
18 HD 50064 Em* 06 51 34.1060183287 +00 17 50.465846394 8.75 9.06 8.30 7.51 6.88 B6Ie 82 1
19 NGC 2403 AGN 07 36 51.396 +65 36 09.17 9.31 8.84 8.38 8.19   ~ 1606 1
20 SN 1954J SN* 07 36 56.20 +65 37 52.3   16.3 16.50     SNIIpec? 90 2
21 * l Pup sg* 07 43 48.4687222 -28 57 17.372015 4.06 4.09 3.93 3.68 3.50 A4Iabe 175 0
22 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2198 0
23 SN 2000ch SN* 10 52 41.40 +36 40 09.5     17.4     SNIIn? 83 2
24 HD 94878 bL* 10 55 58.9150038252 -60 23 33.434805592 8.67 9.37 8.70 8.07   B0/2eq 139 0
25 V* AG Car WR* 10 56 11.5779283438 -60 27 12.809532379 7.00 7.57 6.96 7.73   WN11h 590 0
26 IGR J16318-4848 HXB 16 31 48.3102815892 -48 49 00.664215918           ~ 157 0
27 Cl* Westerlund 1 W 9 WR* 16 47 04.1422943113 -45 50 31.307461802   21.8 17.47 14.47 11.74 Be 46 0
28 * zet01 Sco s*b 16 53 59.7270104119 -42 21 43.313745214 4.80 5.31 4.79 4.32 3.86 B1Ia-0ek 347 0
29 SN 2010mc SN* 17 21 30.68 +48 07 47.4           SNIIn 61 1
30 V* RY Sct Be* 18 25 31.4772031860 -12 41 24.196044092 10.25 10.38 9.12 9.46   O9.7Ibep 284 1
31 EM* MWC 300 Ae* 18 29 25.6915000349 -06 04 37.289920628 12.55 12.67 13.795     B1Ia+[e] 127 0
32 IRAS 18576+0341 s*b 19 00 10.89456 +03 45 47.1096           B8I 80 1
33 SS 433 HXB 19 11 49.5645897701 +04 58 57.824087535   16.3 13.0     A7Ib: 1928 3
34 * P Cyg s*b 20 17 47.2020844 +38 01 58.552724 4.66 5.24 4.82 4.28 4.02 B1-2Ia-0ep 1130 1
35 SN 2009ip s*b 22 23 08.26 -28 56 52.4           LBV 265 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-04:26:08

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