Interstellar and nebular lines toward the 30 Doradus central object

1980 ◽  
Vol 235 ◽  
pp. L101 ◽  
Author(s):  
N. R. Walborn
Keyword(s):  
1983 ◽  
Vol 272 ◽  
pp. 123 ◽  
Author(s):  
N. Panagia ◽  
E. G. Tanzi ◽  
M. Tarenghi

1982 ◽  
Vol 99 ◽  
pp. 231-235
Author(s):  
N. Panagia ◽  
E.G. Tanzi ◽  
M. Tarenghi

We report here on preliminary infrared photometry of six WN stars in the Large Magellanic Cloud. Besides R136, the central object of the 30 Doradus Nebula, the sample includes three stars (R139, R140, R145) located near the center of the region (within ∼ 1 arcmin) and two more stars (R144, R147) at a distance of ∼ 5 arcmin from R136.


1984 ◽  
Vol 108 ◽  
pp. 261-261
Author(s):  
W. Seggewiss ◽  
A.F.J. Moffat

R136 = HD 38268 is the luminous and diffuse central object (V ~ 10m in a region of 7 arc sec diameter) of the young populous cluster NGC 2070 at the centre of the giant H II region 30 Doradus.


1983 ◽  
Vol 273 ◽  
pp. 597 ◽  
Author(s):  
B. D. Savage ◽  
E. L. Fitzpatrick ◽  
J. P. Cassinelli ◽  
D. C. Ebbets
Keyword(s):  

1982 ◽  
Vol 99 ◽  
pp. 563-565
Author(s):  
Joseph P. Cassinelli ◽  
John S. Mathis ◽  
Blair D. Savage

The 30 Doradus nebula is the brightest H II region in the local group. Radio continuum and Radio recombination line observations indicate that it is photoionized by the equivalent of ∼100 05 stars. Observations of the central object R136 made at low and high spectral resolution with the IUE reveal a peculiar hot object with a massive stellar wind. An outflow speed of 3500 kilometers per second and a temperature of approximately 60,000 K are indicated by the spectra. The bulk of the observed ultraviolet radiation must come from R136a, the brightest and bluest component of R136. Its absolute visual magnitude and observed temperature imply a luminosity about 108 times that of the sun. Most of the ionizations produced in 30 Doradus are provided by this peculiar object. If R136a is a dense cluster of very hot stars, about 30 stars of classes 03 and WN3 exist in a region estimated to have a diameter of less than 0.1 parsec. This is inconsistent with the ultraviolet line spectrum and the evidence for optical variability. An alternative interpretation of the observations is that the radiation from R136a is dominated by a single super-luminous object with the following approximate properties: luminosity and temperature as given above, a radius 100 times that of the sun, a mass 2500 times that of the sun, and a loss rate of 10−3.5 solar masses per year. Model interior calculations for hydrogen-burning stars are consistent with these parameters. Such stars, however, are expected to be unstable, and this may account for the massive stellar wind.


Science ◽  
1981 ◽  
Vol 212 (4502) ◽  
pp. 1497-1501 ◽  
Author(s):  
J. P. CASSINELLI ◽  
J. S. MATHIS ◽  
B. D. SAVAGE
Keyword(s):  

Author(s):  
Joseph P. Cassinelli ◽  
John S. Mathis ◽  
Blair D. Savage
Keyword(s):  

1991 ◽  
Vol 378 ◽  
pp. L21 ◽  
Author(s):  
G. Weigelt ◽  
R. Albrecht ◽  
C. Barbieri ◽  
J. C. Blades ◽  
A. Boksenberg ◽  
...  

1999 ◽  
Vol 117 (1) ◽  
pp. 225-237 ◽  
Author(s):  
Nolan R. Walborn ◽  
Rodolfo H. Barbá ◽  
Wolfgang Brandner ◽  
Mónica Rubio ◽  
Eva K. Grebel ◽  
...  
Keyword(s):  

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