2010A&A...524A..82L


Query : 2010A&A...524A..82L

2010A&A...524A..82L - Astronomy and Astrophysics, volume 524, A82-82 (2010/12-1)

The Quintuplet cluster. II. Analysis of the WN stars.

LIERMANN A., HAMANN W.-R., OSKINOVA L.M., TODT H. and BUTLER K.

Abstract (from CDS):

Based on K-band integral-field spectroscopy, we analyze four Wolf-Rayet stars of the nitrogen sequence (WN) found in the inner part of the Quintuplet cluster. All WN stars (WR102d, WR102i, WR102hb, and WR102ea) are of spectral subtype WN9h. One further star, LHO110, is included in the analysis which has been classified as Of/WN? previously but turns out to be most likely a WN9h star as well. The Potsdam Wolf-Rayet (PoWR) models for expanding atmospheres are used to derive the fundamental stellar and wind parameters. The stars turn out to be very luminous, log(L/L)>6.0, with relatively low stellar temperatures, T*≃25-35kK. Their stellar winds contain a significant fraction of hydrogen, up to XH∼0.45 (by mass). We discuss the position of the Galactic center WN stars in the Hertzsprung-Russell diagram and find that they form a distinct group. In this respect, the Quintuplet WN stars are similar to late-type WN stars found in the Arches cluster and elsewhere in the Galaxy. Comparison with stellar evolutionary models reveals that the Quintuplet WN stars should have been initially more massive than 60M. They are about 2.4-3.6 million years old, and might still be central hydrogen burning objects. The analysis of the spectral energy distributions of the program stars results in a mean extinction of AK=3.1±0.5mag (AV=27±4mag) towards the Quintuplet cluster.

Abstract Copyright:

Journal keyword(s): open clusters and associations: individual: Quintuplet - stars: Wolf-Rayet - stars: winds, outflows - stars: evolution - stars: atmospheres

Simbad objects: 31

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Number of rows : 31
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 HD 90177 s*b 10 22 53.8430096928 -59 37 28.363616256 9.16 9.66 8 8.15   LBV 320 0
2 V* AG Car WR* 10 56 11.5781414448 -60 27 12.810673260 7.00 7.57 6.96 7.73   WN11h 613 0
3 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 511 0
4 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 13083 0
5 NAME Sgr A* X 17 45 40.03599 -29 00 28.1699           ~ 3928 3
6 WR 102aa WR* 17 45 49.71 -28 49 25.4           WN8-9 24 0
7 WR 102ad WR* 17 45 50.22 -28 49 21.9           WN8-9 24 0
8 WR 102ae WR* 17 45 50.28 -28 49 11.4           WN9h 35 0
9 WR 102af WR* 17 45 50.290 -28 49 17.20           WN7-8 17 0
10 WR 102ag WR* 17 45 50.40 -28 49 20.9           WN8-9 21 0
11 WR 102ah WR* 17 45 50.43 -28 49 21.9           WN8-9h 31 0
12 WR 102ai WR* 17 45 50.47 -28 49 31.5           WN8-9 17 0
13 WR 102aj WR* 17 45 50.48 -28 49 19.2           WN8-9h 26 0
14 NAME Arches Cluster Cl* 17 45 50.5 -28 49 28           ~ 689 0
15 WR 102ak WR* 17 45 50.54 -28 49 20.3           WN8-9 16 0
16 WR 102al WR* 17 45 50.58 -28 49 17.2           WN7-8 24 0
17 WR 102ba WR* 17 45 50.69 -28 49 22.2           WN8-9 16 0
18 WR 102bb WR* 17 45 50.84 -28 49 26.0           WN8-9 19 0
19 WR 102bc WR* 17 45 51.48 -28 49 25.4           WN8 16 0
20 WR 102c WR* 17 46 11.14 -28 49 05.9           WN6 26 1
21 NAME Quintuplet Cluster OpC 17 46 13.9 -28 49 48           ~ 495 0
22 WR 102d WR* 17 46 14.05 -28 49 16.5           WN9 17 0
23 LHO 147 * 17 46 14.27 -28 49 20.0           M0II 2 0
24 GMM 15 s*b 17 46 15.09 -28 49 29.4           O6/8If 17 1
25 LHO 71 WR* 17 46 15.12 -28 49 36.9           WN9 22 0
26 [FMM95] 3 s*b 17 46 15.240 -28 50 03.58           LBV 146 1
27 LHO 67 WR* 17 46 15.940 -28 49 38.05           WN9 20 0
28 WR 102i WR* 17 46 16.54 -28 49 32.0           WN9 14 0
29 NSV 23780 V* 17 46 16.58664 -28 49 49.8756           ~ 21 0
30 [GMC99] D6 s*b 17 46 17.982 -28 49 03.46           LBV 60 0
31 WR 102ka WR* 17 46 18.12 -29 01 36.6           WN10 30 0

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2022.08.09-02:45:30

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