Results 21 to 30 of about 37,244 (118)
Pulsation in extremely low mass helium stars [PDF]
Monthly Notices of the Royal Astronomical Society, 2013 AbstractWe explore the stability of extremely low-mass stars (M < 0.25 M⊙) across a wide range of composition, effective temperature, and luminosity. We identify the instability boundaries associated with radial oscillations. These are a strong function of both composition and radial order (0 ≤ n ≤ 13).
C. S. Jeffery, H. Saio
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Final Evolution of a Low-Mass Star. I
The Astrophysical Journal, 1970 Low mass star evolution from helium burning to white dwarf, describing red giant and mass loss stages in ...
William K. Rose, Richard L. Smith
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On the Rotational Evolution of Young Low‐Mass Stars
The Astrophysical Journal, 1997 Observations of young clusters indicate that a significant fraction of solar-type stars are rotating very slowly, with equatorial velocities less than 10 km s-1. So far, models have failed to reproduce a sufficiently large proportion of these stars on the zero-age main sequence.
Siess, Lionel, Livio, Mario
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Olivier Chesneau's Work on Low Mass Stars [PDF]
EAS Publications Series, 2015 During his too short career, Olivier Chesneau pioneered the study of the circumstellar environments of low mass evolved stars using very high angular resolution techniques. He applied state of the art high angular resolution techniques, such as optical interferometry and adaptive optics imaging, to the the study of a variety of objects, from AGB stars ...
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Testing the Paradigm of Low Mass Star Formation [PDF]
Symposium - International Astronomical Union, 2004 Protostellar core formation is probably much more dynamic, and magnetic fields are probably much less important, than has been previously assumed in the standard model of low-mass star formation. This revised picture has important consequences: it is easier to understand the observed rapidity of star formation in molecular clouds; cores are more likely
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The Formation of Low-Mass Stars and Brown Dwarfs [PDF]
, 2014 It is estimated that ~60% of all stars (including brown dwarfs) have masses below 0.2Msun. Currently, there is no consensus on how these objects form. I will briefly review the four main theories for the formation of low-mass objects: turbulent fragmentation, ejection of protostellar embryos, disc fragmentation, and photo-erosion of prestellar cores. I
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Stochastic analysis of compact stars under composite polytropes. [PDF]
Sci RepNouh MI +3 more
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Star-Like Microgels vs Star Polymers: Similarities and Differences. [PDF]
MacromoleculesPapetti T +3 more
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A universal brown dwarf desert formed between planets and stars. [PDF]
Proc Natl Acad Sci U S ACui K +12 more
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