stars: evolution
Tidal dissipation in stars and fluid planetary layers and its impact on the evolution of star-planet systems
... in stars and planets is one of the key physical mechanisms that drive the evolution of planetary ...orbital/spin evolution of stars, planets and satellites by converting the kinetic energy of ...
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Evolution Of Stars By Kinetic Theory And Quantum Physics On The Basis Generalized Special Relativity
... star evolution by the pressure force and the force of gravity. For stars one have tow forces, pressure force which counter balance the gravity force, thus ...
11
Formation and Evolution of Neutron Star Binaries: Masses of Neutron Stars
... independent of the maximum mass of NS, but the result of evolution of NS binaries. We discuss that NS-NS binaries are formed when the initial mass di ff erence of two progenitors of double neutron stars is ...
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The formation, evolution, and survivability of discs around young binary stars
... this evolution, and the planet would migrate to a higher ...tidal evolution of close binaries can expand the region of instability to the region where planets might ...
196
Low-mass stars: Open problems all along their evolution
... low-mass stars settle on the horizontal branch (or the clump, depending on their composition and mass) and experience a quiet phase of convective core helium ...the evolution of the convective regions is ...
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Star/disk interaction and angular momentum evolution model for solar-like stars
... momentum evolution of young suns such as the magnetospheric ejection process (hereafter MEP, [10]) that describes the magnetic interaction between a stellar magnetosphere and an accretion disk, and the accretion ...
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Evolution of Neutron Stars and Observational Constraints
... and evolution of neutron stars is discussed with a view towards constraining the prop- erties of high density matter through ...neutron stars is illuminated through the use of several analytical ...
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Spectra of Earth like planets through geological evolution around FGKM stars
... significant evolution since forma- tion (Walker ...Sun-like stars (F0V - M8V) using a self-consistent climate and photochemistry model and a solar evolution model (Claire et ...
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Evolution and fate of very massive stars
... their evolution is not so much affected by rotational mixing, but more by mass loss through stellar ...Their evolution is never far from a homogeneous evolution even without rotational ...these ...
19
Selected topics in the evolution of low-mass stars
... The evolution of a “typical” (single) low-mass star accross the Hertzsprung-Russell diagram, from the zero-age main sequence (ZAMS) to the white dwarf (WD) cooling curve, is shown in Figure ...the evolution ...
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Non-linear evolution of the tidal elliptical instability in gaseous planets and stars
... Tidally distorted rotating stars and gaseous planets are subject to a well-known linear fluid instability – the elliptical instability. It has been proposed that this instability might drive enough energy ...
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Precision diagnostics of pulsation and evolution in helium rich low mass stars
... subdwarf stars, provid- ing spectroscopic classifications for 5055 hot subdwarfs, 540 of which are ...2122 stars with spectra in the SDSS ...helium-rich stars such as He-sdOs, RVs of such ...
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Why is "The Evolution of Stars" incorrect?
... of stars and other objects inside the galaxy and ...other stars, galaxies and clusters of galaxies, it is not difficult to conclude that the old theories are completely wrong and badly conceived mind ...
6
Li abundances in F stars : planets, rotation, and Galactic evolution
... hotter stars, probably because of their shallower convective ...of stars hosting hot jupiters since these planets are massive and some theories of planet formation pre- dict a migration close to the star ...
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The Formation and Evolution of Neutron Stars: Astrometry, Timing, and Transients
... The discovery of ‘SGR-like’ outbursts from 1E 2259+586 was the first direct ev- idence of the connection between SGRs and AXPs (Kaspi et al. 2003). However, the nature of the relation based on indirect evidence, such as ...
162
Modelling transport processes in stellar radiative interiors
... late-B stars, all spectral types well known for harbouring numerous classes of chemical peculiar ...stellar evolution codes because it requires the costly computation of the ra- diative accelerations based ...
6
Asteroseismic Constraints on the Models of Hot B Subdwarfs: Convective Helium-Burning Cores
... stellar evolution models seem to be inade- quate during the phase of ...clump stars to stellar evolution ...main-sequence evolution [92, 93], a consistent picture might well emerge in the ...
10
A circumbinary debris disk in a polluted white dwarf system
... and evolution of planetary systems around close binary stars is a challenging problem, yet provides insight into the growth of planetesimals within evolving protoplanetary disks and planet formation in ...
25
The EBLM Project V Physical properties of ten fully convective, very low mass stars
... stellar evolution models: the radii of low-mass stars are frequently inflated with respect to stellar mod- els, by up to 20% ...low-mass stars, with good agreement between effective temperatures and ...
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The eleventh and twelfth data releases of the Sloan Digital Sky Survey : final data from SDSS III
... of stars as part of the Apache Point Observatory ( APO ) Galactic Evolution Experiment ( APOGEE ) , and includes repeated accurate radial velocity measurements of 5500 stars from the Multi-object APO ...
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