Main Sequence Angular Momentum Loss in Low-Mass Stars

1991 ◽  
pp. 151-165 ◽  
Author(s):  
David R. Soderblom
Keyword(s):  
Angular Momentum ◽  
Main Sequence ◽  
Low Mass Stars ◽  
Momentum Loss ◽  
Angular Momentum Loss ◽  
Low Mass

scholarly journals A nonextensive approach for the angular momentum loss rate in low-mass stars

2012 ◽  
Vol 8 (S294) ◽  
pp. 197-198
Author(s):  
Daniel B. de Freitas ◽  
J. R. De Medeiros
Keyword(s):  
Angular Momentum ◽  
Loss Rate ◽  
Rotational Velocity ◽  
Low Mass Stars ◽  
New Approach ◽  
Momentum Loss ◽  
Angular Momentum Loss ◽  
Low Mass

AbstractThe present study demonstrates that behavior of rotational velocity as a function of stellar age is consistent using Tsallis' nonextensive formalism, resulting in a new approach to understanding the stellar rotational scenario.

scholarly journals The rotational evolution of young low mass stars

2007 ◽  
Vol 3 (S243) ◽  
pp. 231-240 ◽  
Author(s):  
Jérôme Bouvier
Keyword(s):  
Angular Momentum ◽  
Accretion Disk ◽  
Main Sequence ◽  
Young Stars ◽  
Sequence Evolution ◽  
Main Sequence Stars ◽  
Low Mass Stars ◽  
Rotational Evolution ◽  
Low Mass

AbstractStar-disk interaction is thought to drive the angular momentum evolution of young stars. In this review, I present the latest results obtained on the rotational properties of low mass and very low mass pre-main sequence stars. I discuss the evidence for extremely efficient angular momentum removal over the first few Myr of pre-main sequence evolution and describe recent results that support an accretion-driven braking mechanism. Angular momentum evolution models are presented and their implication for accretion disk lifetimes discussed.

scholarly journals The rotation of very low-mass stars and brown dwarfs

2007 ◽  
Vol 3 (S243) ◽  
pp. 241-248
Author(s):  
Jochen Eislöffel ◽  
Alexander Scholz
Keyword(s):  
Angular Momentum ◽  
Brown Dwarfs ◽  
Magnetic Interaction ◽  
Stellar Winds ◽  
Solar Mass ◽  
Low Mass Stars ◽  
Angular Momentum Loss ◽  
Rotational Evolution ◽  
Solar Type ◽  
Low Mass

AbstractThe evolution of angular momentum is a key to our understanding of star formation and stellar evolution. The rotational evolution of solar-mass stars is mostly controlled by magnetic interaction with the circumstellar disc and angular momentum loss through stellar winds. Major differences in the internal structure of very low-mass stars and brown dwarfs – they are believed to be fully convective throughout their lives, and thus should not operate a solar-type dynamo – may lead to major differences in the rotation and activity of these objects. Here, we report on observational studies to understand the rotational evolution of the very low-mass stars and brown dwarfs.

scholarly journals Angular Momentum Loss in Post-Main Sequence Stellar Evolution Through the PN Stage

1993 ◽  
Vol 155 ◽  
pp. 368-368
Author(s):  
M. Villata
Keyword(s):  
Angular Momentum ◽  
Stellar Evolution ◽  
White Dwarf ◽  
Main Sequence ◽  
Sequence Evolution ◽  
Simple Analytical Model ◽  
Momentum Loss ◽  
Angular Momentum Loss ◽  
Pn Stage ◽  
Large Angular Momentum

A simple analytical model can explain the large angular momentum loss which a star suffers in its post-main-sequence evolution up to the white dwarf stage.

scholarly journals Formation and Evolution of Low-Mass Algols

1989 ◽  
Vol 107 ◽  
pp. 141-153
Author(s):  
L.R. Yungelson ◽  
A.V. Tutukov ◽  
A.V. Fedorova
Keyword(s):  
Angular Momentum ◽  
Gravitational Waves ◽  
Stellar Winds ◽  
Momentum Loss ◽  
Angular Momentum Loss ◽  
Low Mass ◽  
Formation And Evolution

AbstractWe discuss the origin, evolution and fate of low-mass Algols (LMA) that have components with initial masses less than 2.5 M0. The semi-major axes of orbits of pre-LMA do not exceed 20-25 R0. The rate of formation of Algol-type stars is ~ 0.01/year. Magnetic stellar winds may be the factor that determines the evolution of LMA. Most LMA end their lives as double helium degenerate dwarfs with M1/M2 ~ 0.88 (like L870-2). Some of them even merge through angular momentum loss caused by gravitational waves.

scholarly journals The Origin and Evolution of Cataclysmic Binaries

1983 ◽  
Vol 72 ◽  
pp. 239-255
Author(s):  
P.P. Eggleton
Keyword(s):  
Angular Momentum ◽  
Significant Loss ◽  
Low Mass Stars ◽  
Tidal Friction ◽  
Origin And Evolution ◽  
Secular Evolution ◽  
Cataclysmic Binaries ◽  
Angular Momentum Loss ◽  
Early Case ◽  
Low Mass

ABSTRACTSome cataclysmic binaries may be products of Case C evolution of low mass stars (orbital period ~ 1 yr; masses ~ 1 - 4 Mʘ), involving a common envelope phase. Other mechanisms, probably involving late Case B and even early Case B, but with significant loss of angular momentum, may be necessary to account for some evolved binaries such as AA Dor or V Sge. Further angular momentum loss, probably by magnetic braking coupled with tidal friction, causes secular evolution in cataclysmic binaries. It is suggested that tidal friction may account for the shortage of cataclysmics with periods ≲ 1.3 hr; but this cutoff, as well as the gap in the period distribution between 2 and 3 hrs, is hard to explain and imposes more severe constraints on possible theories than is commonly acknowledged.

scholarly journals On the Evolutionary History of Progenitors of EHBs and Related Binary Systems from their Observed Properties

2006 ◽  
Vol 2 (S240) ◽  
pp. 678-681
Author(s):  
V.V. Pustynski ◽  
I. Pustylnik
Keyword(s):  
Angular Momentum ◽  
Binary Systems ◽  
Mass Loss Rate ◽  
Analytical Formula ◽  
Solar Mass ◽  
Momentum Loss ◽  
Angular Momentum Loss ◽  
History Of ◽  
Low Mass ◽  
Red Giant

AbstractIt has been shown quite recently (Morales-Rueda et al. 2003) that dB stars, extreme horizontal branch (EHB) objects in high probability all belong to binary systems. We study in detail the mass and angular momentum loss from the giant progenitors of sdB stars in an attempt to clarify why binarity must be a crucial factor in producing EHB objects. Assuming that the progenitors of EHB objects belong to binaries with initial separations of a roughly a hundred solar radii and fill in their critical Roche lobes while close to the tip of red giant branch, we have found that considerable shrinkage of the orbit can be achieved due to a combined effect of angular momentum loss from the red giant and appreciable accretion on its low mass companion on the hydrodynamical timescale of the donor, resulting in formation of helium WD with masses roughly equal to a half solar mass and thus evading the common envelope stage. A simple approximative analytical formula for mass loss rate from Roche lobe filling giant donor has been proposed depending on mass, luminosity and radius of donor.

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