2015A&A...579A.131C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST04:38:39

2015A&A...579A.131C - Astronomy and Astrophysics, volume 579A, 131-131 (2015/7-1)

The VLT-FLAMES Tarantula survey. XX. The nature of the X-ray bright emission-line star VFTS 399.

CLARK J.S., BARTLETT E.S., BROOS P.S., TOWNSLEY L.K., TAYLOR W.D., WALBORN N.R., BIRD A.J., SANA H., DE MINK S.E., DUFTON P.L., EVANS C.J., LANGER N., MAIZ-APELLANIZ J., SCHNEIDER F.R.N. and SOSZYNSKI I.

Abstract (from CDS):

The stellar population of the 30 Doradus star-forming region in the Large Magellanic Cloud contains a subset of apparently single, rapidly rotating O-type stars. The physical processes leading to the formation of this cohort are currently uncertain. One member of this group, the late O-type star VFTS399, is found to be unexpectedly X-ray bright for its bolometric luminosity - in this study we aim to determine its physical nature and the cause of this behaviour. To accomplish this we performed a time-resolved analysis of optical, infrared and X-ray observations. We found VFTS399 to be an aperiodic photometric variable with an apparent near-IR excess. Its optical spectrum demonstrates complex emission profiles in the lower Balmer series and select HeI lines - taken together these suggest an OeBe classification. The highly variable X-ray luminosity is too great to be produced by a single star, while the hard, non-thermal nature suggests the presence of an accreting relativistic companion. Finally, the detection of periodic modulation of the X-ray lightcurve is most naturally explained under the assumption that the accretor is a neutron star. VFTS399 appears to be the first high-mass X-ray binary identified within 30 Dor, sharing many observational characteristics with classical Be X-ray binaries. Comparison of the current properties of VFTS399 to binary-evolution models suggests a progenitor mass>25M for the putative neutron star, which may host a magnetic field comparable in strength to those of magnetars. VFTS399 is now the second member of the cohort of rapidly rotating ``single'' O-type stars in 30 Dor to show evidence of binary interaction resulting in spin-up, suggesting that this may be a viable evolutionary pathway for the formation of a subset of this stellar population.

Abstract Copyright:

Journal keyword(s): stars: emission-line, Be - binaries: general - stars: individual: VFTS399

CDS comments: Paragraph 5 LS I +63 325 misprint not identified. Paragraph 3.2 CXO J1745-28 not identified (incomplete format).

Simbad objects: 30

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Number of rows : 30

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 BD+60 73 HXB 00 37 09.6358465128 +61 21 36.485521705 9.79 10.14 9.66     B1Ib 62 0
2 V* V662 Cas HXB 01 18 02.6973905772 +65 17 29.829417242 12.27 11.99 11.14 10.33 9.58 B1Iae 231 0
3 Ass Cas OB 8 As* 01 44 +61.1           ~ 43 0
4 NGC 663 OpC 01 46 09 +61 14.1   7.78 7.1     ~ 235 0
5 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5665 1
6 PSR J0348+0432 Psr 03 48 43.6365407296 +04 32 11.460202882           ~ 147 1
7 V* X Per HXB 03 55 23.0778791365 +31 02 45.045745259 6.090 6.840 6.720     O9.5III 901 0
8 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
9 VFTS 5 * 05 37 01.7367724164 -69 08 16.284819322   16.27 16.25     B2V(n) 6 0
10 UCAC2 1803231 * 05 37 39.2305260100 -69 09 51.024963212 15.220 16.099 15.806 16.07 15.118 O9:Vnnne+ 23 0
11 PSR J0537-6910 Psr 05 37 46.66 -69 10 17.1           ~ 228 1
12 2MASS J05382624-6905019 * 05 38 26.2230109292 -69 05 01.820560677 13.996 14.810 14.826   14.992 O9.5IV(n) 8 0
13 VFTS 399 * 05 38 33.410 -69 11 59.05   15.91 15.83     O9IIIn 10 0
14 2MASS J05383341-6911588 X 05 38 33.42 -69 11 58.9           ~ 5 0
15 RMC 140a WR* 05 38 41.600 -69 05 13.39   12.18 12.12   12.40 WN4+WC5 31 0
16 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1734 1
17 BAT99 112 WR* 05 38 42.9162 -69 06 04.938   12.95 12.86     WN5h 48 0
18 HD 245770 HXB 05 38 54.5749436467 +26 18 56.839215267 9.30 9.84 9.39 8.77 8.30 O9/B0III/Ve 870 0
19 Mrk 34 Sy2 10 34 08.606 +60 01 52.33   15.71 14.65     ~ 212 1
20 HD 93162 WR* 10 44 10.3888220947 -59 43 11.105959983 7.90 8.55 8.80 8.66   O2.5If*/WN6+OB 334 1
21 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2201 0
22 Ass Cen OB 1 As* 13 02 -61.4           ~ 102 0
23 CPD-63 2495 HXB 13 02 47.6541729595 -63 50 08.625922862 10.34 10.72 9.98 10.03   O9.5Ve 674 1
24 WR 48a WR* 13 12 39.65 -62 42 55.8           WC6 77 0
25 HD 153919 HXB 17 03 56.7728262865 -37 50 38.912077679 6.06 6.78 6.51 6.08 5.90 O6Iafcp 756 1
26 NAME Duck Redux Rad 18 02 10.000 -24 54 00.00           ~ 168 3
27 BD+53 2790 HXB 22 07 56.2368407539 +54 31 06.405811141 9.4 10.11 9.84 9.64 9.43 O9.5Vep 173 0
28 HD 215227 Be* 22 42 57.30295 +44 43 18.2525 8.07 8.86 8.81     B1.5-B2III 79 1
29 * omi And Be* 23 01 55.2645930 +42 19 33.533383 3.00 3.53 3.62 3.61 3.69 B6IV/V_sh 411 0
30 NAME Local Group GrG ~ ~           ~ 6970 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-04:38:39

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