Results 191 to 200 of about 38,720 (218)

The Evolution of Low-Mass Stars

1995
We 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, 1967
Evolutionary 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 Quark Stars

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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The Evolution of Low-Mass Stars

1992
At 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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Opacity problems in cool low mass stars

International Astronomical Union Colloquium, 1994
In this contribution we want to discuss M star atmospheres and their dependence on molecular opacities. A star belongs to the spectral class M if its optical and infrared spectrum shows strong bands of TiO and numerous strong metal lines so that for wavelengths < 4000 Å there is “hardly any flux left” (Jaschek & Jaschek 1987).
Michael Scholz, Rainer Wehrse
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A low-mass star with a large-mass planet

Science, 2023
A large planet orbiting a very low-mass star challenges theories of planet ...
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The Formation of Low Mass Stars

1999
The- 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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Low-Mass Stars and Their Companions

2017
In 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

Publications of the Astronomical Society of the Pacific, 1989
Visible 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, 1988
A 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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