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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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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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The Evolution of Low-Mass Stars
1992At the end of core hydrogen burning low-mass stars develop a helium core where the electrons are degenerate. This occurs when the mass of this helium core is smaller than 0.31 M⊙. The upper boundary for this group of low-mass stars is not exactly determined; in fact it depends on the initial chemical composition of the stars and on the details of the ...
C. W. H. De Loore, C. Doom
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Low-Mass Stars and Their Companions
2017In this thesis, I present seven studies aimed towards better understanding the demographics and physical properties of M dwarfs and their companions. These studies focus in turn on planetary, brown dwarf, and stellar companions to M dwarfs. I begin with an analysis of radial velocity and transit timing analyses of multi-transiting planetary systems ...
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Mass Determination of Very Low Mass Stars
1995We discuss the precision achieved with the present observing techniques for the mass determination of low and very low mass stars. We show the gain that will be achieved with high precision radial velocity measurements combined with diffraction-limited imaging with 8-m class telescopes and the VLTI.
A. Duquennoy +3 more
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