scholarly journals The Stellar Population of R136

1999 ◽  
Vol 190 ◽  
pp. 217-221
Author(s):  
Deidre A. Hunter
Keyword(s):  
Stellar Population ◽  
Massive Stars ◽  
Compact Star ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Cluster

The luminous, compact star cluster R136 in the Large Magellanic Cloud is 300 times more spatially concentrated than a typical OB association and contains at least 39 O3 stars, the most massive of which is ~150 M⊙. Yet, the stellar IMF for 2.8–120 M⊙ is normal. The massive stars are 1–2 Myrs old, and Wolf-Rayet stars are not evolved.

scholarly journals GHRS Observations of Massive Stars in the Large Magellanic Cloud

1992 ◽  
Vol 9 ◽  
pp. 475-476
Author(s):  
Steven N. Shore
Keyword(s):  
High Resolution ◽  
Stellar Population ◽  
Massive Stars ◽  
Photon Counting ◽  
High Sensitivity ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Hot Stars ◽  
Atomic Transitions ◽  
Space Observations

Hot stars are the natural targets for ultraviolet space observations. The bulk of their energy emerges shortward of the atmospheric cutoff and nearly all of the important atomic transitions required for their analysis are located in the region shortward of λ3000Å. However, since they are intrinsically rare, reddening and distance conspire to make the job of studying these important members of the stellar population of a galaxy a very difficulty task. The Goddard High Resolution Spectrograph (GHRS) adds the new dimension of photon counting to high sensitivity and resolution. This means that the massive stars can be more easily observed within our Galaxy, and also in other galaxies.

Infrared Studies of the Young Stellar Population of 30 Doradus

1980 ◽  
Vol 4 (1) ◽  
pp. 90-92
Author(s):  
P. J. McGregor ◽  
A. R. Hyland
Keyword(s):  
Star Formation ◽  
Stellar Population ◽  
Cluster Formation ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Formation Processes ◽  
Excellent Opportunity ◽  
Infrared Studies ◽  
30 Doradus

The 30 Doradus region offers an excellent opportunity to study cluster formation processes and recent star formation in the Large Magellanic Cloud.

scholarly journals The VLT–FLAMES Tarantula Survey

2009 ◽  
Vol 5 (S266) ◽  
pp. 35-40 ◽  
Author(s):  
C. J. Evans ◽  
N. Bastian ◽  
Y. Beletsky ◽  
I. Brott ◽  
M. Cantiello ◽  
...  
Keyword(s):  
Quantitative Analysis ◽  
Massive Stars ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Cluster Evolution ◽  
30 Doradus

AbstractThe Tarantula Survey is an ambitious ESO Large Programme that has obtained multi-epoch spectroscopy of over 1000 massive stars in the 30 Doradus region in the Large Magellanic Cloud. Here, we introduce the scientific motivations of the survey and give an overview of the observational sample. Ultimately, quantitative analysis of every star, paying particular attention to the effects of rotational mixing and binarity, will be used to address fundamental questions in both stellar and cluster evolution.

scholarly journals A VLT/FLAMES STUDY OF THE PECULIAR INTERMEDIATE-AGE LARGE MAGELLANIC CLOUD STAR CLUSTER NGC 1846. I. KINEMATICS

2012 ◽  
Vol 762 (1) ◽  
pp. 65 ◽  
Author(s):  
A. D. Mackey ◽  
G. S. Da Costa ◽  
A. M. N. Ferguson ◽  
D. Yong
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Cluster

scholarly journals DEEP WASHINGTON PHOTOMETRY OF INCONSPICUOUS STAR CLUSTER CANDIDATES IN THE LARGE MAGELLANIC CLOUD

2015 ◽  
Vol 149 (2) ◽  
pp. 52 ◽  
Author(s):  
Samyaday Choudhury ◽  
Annapurni Subramaniam ◽  
Andrés E. Piatti
Keyword(s):  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Star Cluster

scholarly journals The Wolf–Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud

2019 ◽  
Vol 627 ◽  
pp. A151 ◽  
Author(s):  
T. Shenar ◽  
D. P. Sablowski ◽  
R. Hainich ◽  
H. Todt ◽  
A. F. J. Moffat ◽  
...  
Keyword(s):  
Mass Loss ◽  
Stellar Evolution ◽  
Massive Stars ◽  
Large Magellanic Cloud ◽  
Magellanic Cloud ◽  
Binary Interaction ◽  
Evolutionary Status ◽  
X Ray ◽  
Composite Spectra ◽  
The Impact

Context. Massive Wolf–Rayet (WR) stars dominate the radiative and mechanical energy budget of galaxies and probe a critical phase in the evolution of massive stars prior to core collapse. It is not known whether core He-burning WR stars (classical WR; cWR) form predominantly through wind stripping (w-WR) or binary stripping (b-WR). Whereas spectroscopy of WR binaries has so-far largely been avoided because of its complexity, our study focuses on the 44 WR binaries and binary candidates of the Large Magellanic Cloud (LMC; metallicity Z ≈ 0.5 Z⊙), which were identified on the basis of radial velocity variations, composite spectra, or high X-ray luminosities. Aims. Relying on a diverse spectroscopic database, we aim to derive the physical and orbital parameters of our targets, confronting evolution models of evolved massive stars at subsolar metallicity and constraining the impact of binary interaction in forming these stars. Methods. Spectroscopy was performed using the Potsdam Wolf–Rayet (PoWR) code and cross-correlation techniques. Disentanglement was performed using the code Spectangular or the shift-and-add algorithm. Evolutionary status was interpreted using the Binary Population and Spectral Synthesis (BPASS) code, exploring binary interaction and chemically homogeneous evolution. Results. Among our sample, 28/44 objects show composite spectra and are analyzed as such. An additional five targets show periodically moving WR primaries but no detected companions (SB1); two (BAT99 99 and 112) are potential WR + compact-object candidates owing to their high X-ray luminosities. We cannot confirm the binary nature of the remaining 11 candidates. About two-thirds of the WN components in binaries are identified as cWR, and one-third as hydrogen-burning WR stars. We establish metallicity-dependent mass-loss recipes, which broadly agree with those recently derived for single WN stars, and in which so-called WN3/O3 stars are clear outliers. We estimate that 45  ±  30% of the cWR stars in our sample have interacted with a companion via mass transfer. However, only ≈12  ±  7% of the cWR stars in our sample naively appear to have formed purely owing to stripping via a companion (12% b-WR). Assuming that apparently single WR stars truly formed as single stars, this comprises ≈4% of the whole LMC WN population, which is about ten times less than expected. No obvious differences in the properties of single and binary WN stars, whose luminosities extend down to log L ≈ 5.2 [L⊙], are apparent. With the exception of a few systems (BAT99 19, 49, and 103), the equatorial rotational velocities of the OB-type companions are moderate (veq ≲ 250 km s−1) and challenge standard formalisms of angular-momentum accretion. For most objects, chemically homogeneous evolution can be rejected for the secondary, but not for the WR progenitor. Conclusions. No obvious dichotomy in the locations of apparently single and binary WN stars on the Hertzsprung-Russell diagram is apparent. According to commonly used stellar evolution models (BPASS, Geneva), most apparently single WN stars could not have formed as single stars, implying that they were stripped by an undetected companion. Otherwise, it must follow that pre-WR mass-loss/mixing (e.g., during the red supergiant phase) are strongly underestimated in standard stellar evolution models.

Discovery of a Luminous White Dwarf in a Young Star Cluster in the Large Magellanic Cloud

1998 ◽  
Vol 499 (1) ◽  
pp. L53-L56 ◽  
Author(s):  
Rebecca A. W. Elson ◽  
Steinn Sigurdsson ◽  
Jarrod Hurley ◽  
Melvyn B. Davies ◽  
Gerard F. Gilmore
Keyword(s):  
White Dwarf ◽  
Large Magellanic Cloud ◽  
Young Star ◽  
Magellanic Cloud ◽  
Star Cluster
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