Difference between revisions of "User:Tohline/Apps/OstrikerBodenheimerLyndenBell66"
| Line 8: | Line 8: | ||
As we have reviewed in an [[User:Tohline/SSC/Structure/WhiteDwarfs#Chandrasekhar_mass|accompanying discussion]], | As we have reviewed in an [[User:Tohline/SSC/Structure/WhiteDwarfs#Chandrasekhar_mass|accompanying discussion]], | ||
[http://adsabs.harvard.edu/abs/1935MNRAS..95..207C Chandrasekhar (1935)] was the first to construct models of spherically symmetric stars using the [[User:Tohline/SR#Time-Independent_Problems|barotropic equation of state appropriate for a degenerate electron gas]]. In so doing, he demonstrated that the maximum mass of an isolated, nonrotating white dwarf is <math>M_3 = 1.44 (\mu_e/2)M_\odot</math> | [http://adsabs.harvard.edu/abs/1935MNRAS..95..207C Chandrasekhar (1935)] was the first to construct models of spherically symmetric stars using the [[User:Tohline/SR#Time-Independent_Problems|barotropic equation of state appropriate for a degenerate electron gas]]. In so doing, he demonstrated that the maximum mass of an isolated, nonrotating white dwarf is <math>M_3 = 1.44 (\mu_e/2)M_\odot</math>. A concise derivation of <math>~M_3</math> is presented in Chapter ''XI'' of [[User:Tohline/Appendix/References#C67|Chandrasekhar (1967)]]. | ||
| Line 18: | Line 18: | ||
<font color="green">In this Letter we demonstrate that white-dwarf models with masses considerably greater than <math>~M_3</math> are possible if differential rotation is allowed … models are based on the physical assumption of an axially symmetric, completely degenerate, self-gravitating fluid, in which the effects of viscosity, magnetic fields, meridional circulation, and relativistic terms in the hydrodynamical equations have been neglected.</font> | <font color="green">In this Letter we demonstrate that white-dwarf models with masses considerably greater than <math>~M_3</math> are possible if differential rotation is allowed … models are based on the physical assumption of an axially symmetric, completely degenerate, self-gravitating fluid, in which the effects of viscosity, magnetic fields, meridional circulation, and relativistic terms in the hydrodynamical equations have been neglected.</font> | ||
</td></tr></table> | </td></tr></table> | ||
=See Also= | =See Also= | ||
Revision as of 02:37, 20 June 2019
Rotationally Flattened White Dwarfs
|
|---|
| | Tiled Menu | Tables of Content | Banner Video | Tohline Home Page | |
Introduction
As we have reviewed in an accompanying discussion, Chandrasekhar (1935) was the first to construct models of spherically symmetric stars using the barotropic equation of state appropriate for a degenerate electron gas. In so doing, he demonstrated that the maximum mass of an isolated, nonrotating white dwarf is <math>M_3 = 1.44 (\mu_e/2)M_\odot</math>. A concise derivation of <math>~M_3</math> is presented in Chapter XI of Chandrasekhar (1967).
- J. P. Ostriker, P. Bodenheimer & D. Lynden-Bell (1966), Phys. Rev. Letters, 17, 816: Equilibrium Models of Differentially Rotating Zero-Temperature Stars
|
… work by Roxburgh (1965, Z. Astrophys., 62, 134), Anand (1965, Proc. Natl. Acad. Sci. U.S., 54, 23), and James (1964, ApJ, 140, 552) shows that the [Chandrasekhar (1931, ApJ, 74, 81)] mass limit <math>~M_3</math> is increased by only a few percent when uniform rotation is included in the models, … In this Letter we demonstrate that white-dwarf models with masses considerably greater than <math>~M_3</math> are possible if differential rotation is allowed … models are based on the physical assumption of an axially symmetric, completely degenerate, self-gravitating fluid, in which the effects of viscosity, magnetic fields, meridional circulation, and relativistic terms in the hydrodynamical equations have been neglected. |
See Also
|
|
|---|
|
© 2014 - 2021 by Joel E. Tohline |