2009A&A...507.1597R


Query : 2009A&A...507.1597R

2009A&A...507.1597R - Astronomy and Astrophysics, volume 507, 1597-1611 (2009/12-1)

Spectroscopic monitoring of the luminous blue variable Westerlund1-243 from 2002 to 2009.

RITCHIE B.W., CLARK J.S., NEGUERUELA I. and NAJARRO F.

Abstract (from CDS):

The massive post-main sequence star W243 in the galactic starburst cluster Westerlund 1 has undergone a spectral transformation from a B2Ia supergiant devoid of emission features in 1981 to an A-type supergiant with a rich emission-line spectrum by 2002/03. We examine the continued evolution of W243 from 2002 to 2009 to understand its evolutionary state, current physical properties and the origin of its peculiar emission line spectrum. We used VLT/UVES and VLT/FLAMES to obtain high resolution, high signal-to-noise spectra on six epochs in 2003/04 (UVES) and ten epochs in 2008/09 (FLAMES). These spectra are used alongside other lower-resolution VLT/FLAMES and NTT/EMMI spectra to follow the evolution of W243 from 2002 to 2009. Non-LTE models are used to determine the physical properties of W243. W243 displays a complex, time-varying spectrum with emission lines of hydrogen, helium and Lyman-α pumped metals, forbidden lines of nitrogen and iron, and a large number of absorption lines from neutral and singly-ionized metals. Many lines are complex emission/absorption blends, with significant spectral evolution occurring on timescales of just a few days. The LBV has a temperature of ∼8500K (spectral type A3Ia+), and displays signs of photospheric pulsations and weak episodic mass loss. Nitrogen is highly overabundant, with carbon and oxygen depleted, indicative of surface CNO-processed material and considerable previous mass-loss, although current time-averaged mass-loss rates are low. The emission-line spectrum forms at large radii, when material lost by the LBV in a previous mass-loss event is ionized by an unseen hot companion. Monitoring of the near-infrared spectrum suggests that the star has not changed significantly since it finished evolving to the cool state, close to the Humphreys-Davidson limit, in early 2003.

Abstract Copyright:

Journal keyword(s): stars: individual: W243 - stars: evolution - supergiants - stars: variables: general - stars: winds, outflows

Simbad objects: 26

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Number of rows : 26
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 SN 2005gl SN* 00 49 50.02 +32 16 56.8       17.0   SNIIn 134 2
2 HD 5980 WR* 00 59 26.5838833944 -72 09 53.927337312   11.13 11.31   11.029 WN4+O7I: 375 1
3 SN 2006gy SN* 03 17 27.06 +41 24 19.5       14.20   SNIIn 316 1
4 V* S Dor sg* 05 18 14.3570612088 -69 15 01.149576912 9.08 10.39 10.25 9.74 9.14 A5Iaeq 364 0
5 SN 1987A SN* 05 35 28.020 -69 16 11.07           SNIIpec 4723 2
6 HD 269858 s*b 05 36 43.6936418088 -69 29 47.451149232   10.24 10.15 9.95 9.05 LBV 277 2
7 HD 90177 s*b 10 22 53.8430096928 -59 37 28.363616256 9.16 9.66 8 8.15   LBV 320 0
8 * eta Car Em* 10 45 03.5377808928 -59 41 04.051599720 6.37 7.03 6.48 4.90 4.41 OBepec 2336 0
9 V* AG Car WR* 10 56 11.5781414448 -60 27 12.810673260 7.00 7.57 6.96 7.73   WN11h 613 0
10 Cl* Westerlund 1 BKS H * 16 47 01.4269856784 -45 50 37.248841536   18.781 14.47     F3Ia+ 26 0
11 Cl* Westerlund 1 W 234 V* 16 47 01.4379463296 -45 52 35.096731572   21.3 17.53 15.25 12.85 O9.5Ib 8 0
12 Cl* Westerlund 1 W 12 sg* 16 47 02.2214295629 -45 50 58.987616665   22.0 17.575 13.611   A5Ia+ 23 0
13 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 511 0
14 Cl* Westerlund 1 W 9 WR* 16 47 04.1419806984 -45 50 31.311670632   21.8 17.47 14.47 11.74 Be 49 0
15 Cl* Westerlund 1 W 265 * 16 47 06.2785465416 -45 49 23.774098692   22.0 17.739   10.54 F1-5Ia+ 22 0
16 Cl* Westerlund 1 W 16 * 16 47 06.6158603112 -45 50 42.186706944   20.5 16.248     A5Ia+ 25 0
17 Cl* Westerlund 1 W 243 s*b 16 47 07.5040736160 -45 52 29.123491188   19.873 15.730     LBV 56 0
18 HD 160529 sg* 17 41 59.0261939376 -33 30 13.704456780 8.17 7.87 6.66 5.50 4.51 A2Ia 192 1
19 [FMM95] 3 s*b 17 46 15.240 -28 50 03.58           LBV 146 1
20 [KMN95] Star A s*b 18 08 40.312 -20 24 41.14           LBV 40 3
21 HD 168607 s*b 18 21 14.8856951904 -16 22 31.763755236 10.23 9.82 8.28 8.55   B9Iaep 182 1
22 HD 168625 s*b 18 21 19.5484021368 -16 22 26.075142156 10.15 9.78 8.37 8.76   B6Iap 268 2
23 IRC +10420 pA* 19 26 48.0979492536 +11 21 16.758531216   13.98 11.66     F8Ia+e 464 0
24 EM* MWC 349A * 20 32 45.5291969760 +40 39 36.651807828           ~ 154 0
25 V* V509 Cas LP* 23 00 05.1012218544 +56 56 43.350876312 8.01 6.68 5.13 3.96 3.11 G4_0 323 0
26 * rho Cas LP* 23 54 23.0325302520 +57 29 57.774737400 7.00 5.85 4.59 3.63 2.89 G2_0 375 0

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2022.08.18-04:14:21

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