Pulsation hydrodynamics of luminous blue variables and pulsation-driven winds

2008 ◽  
pp. 337-344 ◽  
Author(s):  
Joyce A. Guzik ◽  
Arthur N. Cox ◽  
Kate M. Despain ◽  
Michael S. Soukup
Keyword(s):  
Luminous Blue Variables

The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. I. Results from 19 OB Associations in the Magellanic Clouds

2000 ◽  
Vol 119 (5) ◽  
pp. 2214-2241 ◽  
Author(s):  
Philip Massey ◽  
Elizabeth Waterhouse ◽  
Kathleen DeGioia-Eastwood
Keyword(s):  
Magellanic Clouds ◽  
Luminous Blue Variables ◽  
Ob Associations

scholarly journals Evolutionary Changes in LUMINOUS STARS

1998 ◽  
Vol 11 (1) ◽  
pp. 346-346
Author(s):  
E. Zsldos
Keyword(s):  
Light Curve ◽  
19Th Century ◽  
Stellar Evolution ◽  
Colour Change ◽  
Light Curves ◽  
Appreciable Change ◽  
Luminous Blue Variables ◽  
Secular Changes ◽  
Evolutionary Changes ◽  
The 19Th Century

The light curves of luminous stars often show spectacular secular changes which can be connected to stellar evolution. Such events are, e.g. the outbursts of P Cygni in the 17th century and 77 Carinae in the last century. Both stars belong to the Luminous Blue Variables, but these changes are not restricted to blue stars. The light curve of HR 8752 (V509 Cassiopeiae) shows a certain similarity to that of the former two stars. When it was first catalogued in the middle of the 19th century, it had been a 6m star. During 100 years the star showed a secular brightening of lm. A similar yellow hypergiant, p Cassiopeiae produced at least two outbursts this century, though both have smaller amplitudes than it is in the case of the LBVs. Moreover, these yellow variables also have an apparently secular colour change: the B − V colour of HR 8752 is decreasing while that of ρ Cassiopeiae is increasing. In both cases evolutionary changes are possible but one cannot exclude other causes. Besides these well studied stars there are several other yellow hypergiants with promising light curves. One of the most interesting cases seems to be R Puppis, which was discovered to be variable in the last century, but then did not show any appreciable change in the following 70-80 years. In the late 1970s, however, it began to vary once more.

scholarly journals Triggering eruptive mass ejection in luminous blue variables

New Astronomy ◽  
2009 ◽  
Vol 14 (6) ◽  
pp. 539-544 ◽  
Author(s):  
Amos Harpaz ◽  
Noam Soker
Keyword(s):  
Luminous Blue Variables ◽  
Mass Ejection

scholarly journals Effects of fast rotation on the wind of Luminous Blue Variables

2010 ◽  
Vol 6 (S272) ◽  
pp. 56-61
Author(s):  
Jose H. Groh
Keyword(s):  
Near Infrared ◽  
Rotational Velocity ◽  
Spectral Lines ◽  
High Resolution Spectroscopy ◽  
Luminous Blue Variables ◽  
Eta Carinae ◽  
Fast Rotation ◽  
Long Baseline ◽  
Infrared Interferometry ◽  
Fast Rotating

AbstractWhile theoretical studies have long suggested a fast-rotating nature of Luminous Blue Variables (LBVs), observational confirmation of fast rotation was not detected until recently. Here I discuss the diagnostics that have allowed us to constrain the rotational velocity of LBVs: broadening of spectral lines and latitude-dependent variations of the wind density structure. While rotational broadening can be directly detected using high-resolution spectroscopy, long-baseline near-infrared interferometry is needed to directly measure the shape of the latitude-dependent photosphere that forms in a fast-rotating star. In addition, complex 2-D radiative transfer models need to be employed if one's goal is to constrain rotational velocities of LBVs. Here I illustrate how the above methods were able to constrain the rotational velocities of the LBVs AG Carinae, HR Carinae, and Eta Carinae.

scholarly journals Predictions of variable mass loss for Luminous Blue Variables

2002 ◽  
Vol 393 (2) ◽  
pp. 543-553 ◽  
Author(s):  
Jorick S. Vink ◽  
A. de Koter
Keyword(s):  
Mass Loss ◽  
Variable Mass ◽  
Luminous Blue Variables

scholarly journals The first X-ray survey of Galactic luminous blue variables

2012 ◽  
Vol 538 ◽  
pp. A47 ◽  
Author(s):  
Y. Nazé ◽  
G. Rauw ◽  
D. Hutsemékers
Keyword(s):  
X Ray ◽  
Luminous Blue Variables

scholarly journals Massive star evolution: luminous blue variables as unexpected supernova progenitors

2013 ◽  
Vol 550 ◽  
pp. L7 ◽  
Author(s):  
J. H. Groh ◽  
G. Meynet ◽  
S. Ekström
Keyword(s):  
Massive Star ◽  
Luminous Blue Variables ◽  
Star Evolution ◽  
Massive Star Evolution

scholarly journals Massive stars in their death throes

2008 ◽  
Vol 366 (1884) ◽  
pp. 4441-4452 ◽  
Author(s):  
John J Eldridge
Keyword(s):  
Stellar Evolution ◽  
Massive Stars ◽  
Evolution Theory ◽  
Luminous Blue Variables ◽  
Show Evidence ◽  
Red Supergiants ◽  
Working Backwards

The study of the stars that explode as supernovae used to be a forensic study, working backwards from the remnants of the star. This changed in 1987 when the first progenitor star was identified in pre-explosion images. Currently, there are eight detected progenitors with another 21 non-detections, for which only a limit on the pre-explosion luminosity can be placed. This new avenue of supernova research has led to many interesting conclusions, most importantly that the progenitors of the most common supernovae, type IIP, are red supergiants, as theory has long predicted. However, no progenitors have been detected thus far for the hydrogen-free type Ib/c supernovae, which, given the expected progenitors, is an unlikely result. Also, observations have begun to show evidence that luminous blue variables, which are among the most massive stars, may directly explode as supernovae. These results contradict the current stellar evolution theory. This suggests that we may need to update our understanding.

Luminous Blue Variables

Trembling Air ◽  
2018 ◽  
pp. 64-69
Keyword(s):  
Luminous Blue Variables
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