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A low-mass star with a large-mass planet
Science, 2023A large planet orbiting a very low-mass star challenges theories of planet ...
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Searching for Low Mass Stars in the Halo
Astrophysics and Space Science, 1999From microlensing events detected at high galactic latitude as well as from direct measurements of the halo stellar density, estimations of a potential contribution of low mass stars to the mass budget is questioned. Up to now no clear answer has been found for one main reason: the difficulty to observe them in a sufficient volume, which requires deep ...
A.C. Robin, M. Crézé, V. Mohan
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Astrophysics and Space Science, 1994
Low mass stars contribute an important fraction to the mass of our Galaxy. Due to the faintness of these stars a direct investigation of their space distribution and kinematics can be carried out only in the immediate solar neighbourhood. This fact emphasizes the importance of the “Third Catalogue of Nearby Stars” (CNS3) as a probe of the stellar ...
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Low mass stars contribute an important fraction to the mass of our Galaxy. Due to the faintness of these stars a direct investigation of their space distribution and kinematics can be carried out only in the immediate solar neighbourhood. This fact emphasizes the importance of the “Third Catalogue of Nearby Stars” (CNS3) as a probe of the stellar ...
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Origins of life and evolution of the biosphere, 1997
Recent evidence indicates that most low mass stars in the Galaxy (< 5 M [symbol: see text]) form alongside massive stars in clusters embedded in giant molecular clouds. Once their parental gas is removed, the fate of these clusters is to disperse and blend into the field population of the galactic disk.
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Recent evidence indicates that most low mass stars in the Galaxy (< 5 M [symbol: see text]) form alongside massive stars in clusters embedded in giant molecular clouds. Once their parental gas is removed, the fate of these clusters is to disperse and blend into the field population of the galactic disk.
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Annual Review of Astronomy and Astrophysics, 1987
Very low mass (VLM) stars, which we define here somewhat arbitrarily as those with masses ;$ 0.3 M 0' pose some of the more interesting problems in stellar astrophysics. The physics of their envelopes and atmospheres are more complicated and their structures less well modeled than their more massive counterparts.
James Liebert, Ronald G. Probst
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Very low mass (VLM) stars, which we define here somewhat arbitrarily as those with masses ;$ 0.3 M 0' pose some of the more interesting problems in stellar astrophysics. The physics of their envelopes and atmospheres are more complicated and their structures less well modeled than their more massive counterparts.
James Liebert, Ronald G. Probst
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Low- and Intermediate-Mass Stars
2018Energy in stars is provided by nuclear reactions, which, in many cases, produce radioactive nuclei. When stable nuclei are irradiated by a flux of protons or neutrons, capture reactions push stable matter out of stability into the regime of unstable species. The ongoing production of radioactive nuclei in the deep interior of the Sun via proton-capture
Maria Lugaro, Alessandro Chieffi
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The Evolution of Low-Mass Stars
1995We present evolutionary models for low-mass stars using the best currently available physics for the equation of state, the Rosseland mean opacities and the screening factors of thermonuclear reaction rates. We follow the evolution of stars of mass M ≤ 0. 6 M⊙ down to the hydrogen burning minimum mass, with initial metallicity Z=0, 10-3 and 0. 02.
I. Baraffe, G. Chabrier
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EVOLUTION OF STARS OF LOW MASS
Canadian Journal of Physics, 1967Evolutionary sequences of models in the early and main sequence stages have been constructed for stars in the mass range [Formula: see text] with a composition X = 0.739, Z = 0.021. The general behavior of the evolutionary track in the Hertzsprung–Russell diagram is similar to that obtained for medium-mass stars.
Dilhan Ezer, A. G. W. Cameron
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Low Mass Stars with Mass Loss and Low-Luminosity Carbon Star Formation
1987The effects of large carbon enrichments in static stellar envelopes were investigated, using new Los Alamos opacities (including low-temperature carbon and molecular opacities) and including carbon ionizations. To search for the production of low-mass, low-luminosity carbon stars, detailed stellar evolutionary computations were carried out for a grid ...
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Astrophysics and Space Science, 2005
More and more observational hints of quark stars are proposed these years though pulsars are considered conventionally to be normal neutron stars. The existence of low-mass quark stars is a direct consequence of the possibility that pulsar-like stars are actually quark stars, because of the ability that quark matter can confine itself by color ...
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More and more observational hints of quark stars are proposed these years though pulsars are considered conventionally to be normal neutron stars. The existence of low-mass quark stars is a direct consequence of the possibility that pulsar-like stars are actually quark stars, because of the ability that quark matter can confine itself by color ...
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