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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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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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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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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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The Formation of Low Mass Stars
1999The- question of the origin of stars is one of the most fundamental of astronomy. Yet, despite thousands of years of stellar observation, and early speculations by Newton and Laplace, it has only been in the latter part of the present century that the investigation of star formation has become an active discipline of astrophysical research.
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The formation of low-mass stars
Publications of the Astronomical Society of the Pacific, 1989Visible to millimeter wavelength observations of the global and individual aspects of low-mass star formation are discussed. Infrared and millimeter-wave techniques reveal large collections of dust-embedded young stellar objects associated with the densest regions of molecular clouds.
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Plasmon decay into low-mass bosons in stars
Physical Review D, 1988A low-mass boson a, if it couples by a two-photon vertex, can be produced in the plasma decay process ${\ensuremath{\gamma}}_{t}$\ensuremath{\rightarrow}${\ensuremath{\gamma}}_{l}$+a and in the plasma coalescence process ${\ensuremath{\gamma}}_{t}$+${\ensuremath{\gamma}}_{l}$\ensuremath{\rightarrow}a, where ${\ensuremath{\gamma}}_{t}$ and ${\ensuremath{
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