SN 1987A and SN 1993J: Testing stellar evolution theory?

1994 ◽  
Vol 66 (1-4) ◽  
pp. 439-453 ◽  
Author(s):  
Philipp Podsiadlowski
Keyword(s):  
Stellar Evolution ◽  
Evolution Theory ◽  
Sn 1987A

scholarly journals Stellar Evolution in the Upper HRD: Theory

1991 ◽  
Vol 143 ◽  
pp. 431-444
Author(s):  
Norbert Langer
Keyword(s):  
Mass Loss ◽  
Stellar Evolution ◽  
Structure Evolution ◽  
Evolution Theory ◽  
Sn 1987A ◽  
The Impact

Theoretical aspects of the modeling of observable evolutionary phases of massive single stars are reviewed. The SN 1987A progenitor evolution is considered in detail as an example for a star below the WR limit. Formation, structure, evolution, and mass loss of WR stars are discussed, and the impact of supernova research on stellar evolution theory is stressed.

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.

scholarly journals Disentangling discrepancies between stellar evolution theory and sub-solar mass stars

2003 ◽  
Vol 409 (2) ◽  
pp. 611-618 ◽  
Author(s):  
E. Lastennet ◽  
J. Fernandes ◽  
D. Valls-Gabaud ◽  
E. Oblak
Keyword(s):  
Stellar Evolution ◽  
Evolution Theory ◽  
Solar Mass

scholarly journals Supernova searches and rates

2013 ◽  
Vol 9 (S296) ◽  
pp. 37-44
Author(s):  
Enrico Cappellaro
Keyword(s):  
Stellar Evolution ◽  
Rapid Development ◽  
Cosmic Time ◽  
Stellar Populations ◽  
Evolution Theory ◽  
Direct Link ◽  
Local Universe ◽  
Crucial Test

AbstractSupernova statistics, establishing a direct link between stellar populations and explosion scenarios, is a crucial test of stellar evolution theory. Nowadays, a number of SN searches in the local Universe and at high redshifts are allowing observational probes of long standing theoretical scenarios. I will briefly review some of the most interesting results in particular for what concern the evolution with cosmic time of the SN rate, which is one of the topic that in the last few years had a most rapid development.

scholarly journals An Essay on Stellar Oscillations and Evolution

1983 ◽  
Vol 66 ◽  
pp. 457-467
Author(s):  
Icko Iben
Keyword(s):  
Stellar Evolution ◽  
Evolution Theory ◽  
Agb Stars ◽  
Solar Oscillation ◽  
High Luminosity ◽  
Stellar Oscillations ◽  
Classical Cepheids ◽  
Neutrino Fluxes ◽  
Oscillation Characteristics

AbstractIt is cautioned that solar models adjusted in such a way as to achieve a match between theoretical solar oscillation characteristics and observed ones may produce neutrino fluxes inconsistent with the observations and that this is likely to be explicable as a deficiency in modeling that portion of the envelope which is most strongly affected by uncertainties in the treatment of convection. Then follows a summary of how the results of pulsation theory and of stellar evolution theory have been used together to learn about the structure and evolution of RRLyrae stars, classical Cepheids, and high luminosity AGB stars.

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