منابع مشابه
Post-red Supergiants
The yellow hypergiants are found in a stage between the massive Red Supergiants and the Wolf-Rayet stars. This review addresses current issues concerning the evolution of massive stars, concentrating on the transitional postRed Supergiant phase. Few yellow hypergiants are known and even fewer show direct evidence for having evolved off the Red Supergiant branch. Indeed, only two such rare objec...
متن کاملInfrared Photometry of Red Supergiants in Young Clusters in the Magellanic Clouds
We present broad-band infrared photometry for 52 late-type supergiants in the young Magellanic Clouds clusters NGC 330, NGC 1818, NGC 2004 and NGC 2100. Standard models are seen to differ in the temperature they predict for the red supergiant population on the order of 300K. It appears that these differences most probably due to the calibration of the mixing-length parameter, αP , in the outerm...
متن کاملRed Supergiants in the Local Group
Galaxies in the Local Group span a factor of 15 in metallicity, ranging from the super-solar M31 to the Wolf-Lundmark-Melotte (WLM) galaxy, which is the lowest-metallicity (0.1Z⊙) Local Group galaxy currently forming stars. Studies of massive star populations across this broad range of environments have revealed important metallicitydependent evolutionary trends, allowing us to test the accurac...
متن کاملThe Physical Properties of Red Supergiants
Red supergiants (RSGs) are a He-burning phase in the evolution of moderately massive stars (10-25M⊙). For many years, the assumed physical properties of these stars placed them at odds with the predictions of evolutionary theory. We have recently determined new effective temperatures and luminosities for the RSG populations of galaxies with a factor of ∼8 range in metallicity, including the Mil...
متن کاملThe spin-up of contracting red supergiants
We report on a mechanism which may lead to a spinup of the surface of a rotating single star leaving the Hayashi line, which is much stronger than the spin-up expected from the mere contraction of the star. By analyzing rigidly rotating, convective stellar envelopes, we qualitatively work out the mechanism through which these envelopes may be spun up or down by mass loss through their lower or ...
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ژورنال
عنوان ژورنال: Proceedings of the International Astronomical Union
سال: 2015
ISSN: 1743-9213,1743-9221
DOI: 10.1017/s1743921316005858