Evolution Of Rotating Low Mass Stars With Angular-Momentum Loss

The evolutionary behavior of rotating low mass stars has been investigated with angular momentum loss by the magnetic stellar wind through the pre-main sequence and on the zero age main sequence phases. As the stars contract toward the zero age main sequence, angular momentum is removed from the convective envelope under the assumption that initially only the convective envelope is spun down in low mass stars. It is obtained that most of the angular momentum loss occurs prior to reaching the zero age main sequence. By the time of 7 10(8) yr, rotating low mass stars spin down to below 10 km s-1 surface rotational velocities. Hyades cluster data (Stauffer & Hartmann 1986) show almost the same trend with the isochrone of 7 10(8) yr, obtained in the present study.


Dynamics of the neutron star interior
Alpar, MA (1996-10-11)
This lecture summarizes the basic ideas on the dynamics of rotating superfluids in neutron stars (Section 2), and discusses the application to pulsar glitch models (Section 3). In Section 4 the anomalous braking indices of glitching pulsars are shown to agree with the model developed for the interglitch behaviour of the Vela pulsar, indicating possible universality of the dynamics of large glitches. Energy dissipation in the neutron star interior is discussed in Section 5. For an excellent general review of...
Radial and nonradial oscillations in stars with gravitational potential perturbation
Özel, Nesibe; Civelek, Fevziye Rikkat; Department of Physics (2003)
In this study, the linear adiabatic radial and nonradial oscillations of evolutionary stellar model with 1.80M©, representing the star VI 162 Ori, has been investigated. The already working oscillation program with Cowling approximation, which ig nores the Eulerian perturbation in gravitational potential, has been modified to carry out the radial and nonradial linear adiabatic perturbations of stellar mod els using the Eulerian perturbation in gravitational potential. The new set of equations were solved wi...
Early pre-main sequence evolution of low mass stars
Kucuk, I; Kiziloglu, N; Civelek, R (1998-01-01)
Evolution of the gravitational contraction phase of stars having masses 0.3 < M/M. < 1.5 were studied along with deuterium burning. The equation of state developed by Mihalas et al. (1988) and OPAL opacity tables were used in our investigation. The theoretical time Lines were compared with observations.
Pre-Main-Sequence evolution of rotating low-mass stars
Kızıloğlu, Nilgün (Springer Science and Business Media LLC, 1989-4)
The evolutionary behaviour of rotating low-mass stars in the mass range 0.2 and 0.9M ⊙ has been investigated during the pre-Main-Sequence phase. The angular momentum is conserved locally in radiative regions and totally in convective regions, according to a predetermined angular velocity distribution depending on the structure of the star. As the stars contract toward the zero-age Main Sequence, they spin up under the assumption that the angular momentum is conserved during the evolution of the stars. When ...
Magnetic activity and evolution of Algol-type stars - II
SARNA, MAREK; Yerli, Sinan Kaan; Muslimov, A G (1998-07-01)
We examine the possibility of probing dynamo action in mass-losing stars, components of Algol-type binaries, Our analysis is based on the calculation of nonconservative evolution of these systems, We model the systems U Sge and beta Per where the more massive companion fills its Roche lobe at the main sequence (case AB) and where it has a small helium core (early case B) respectively, We show that to maintain evolution of these systems at the late stages which are presumably driven by stellar 'magnetic brak...
Citation Formats
N. KIZILOGLU, “Evolution Of Rotating Low Mass Stars With Angular-Momentum Loss,” ASTRONOMY & ASTROPHYSICS, pp. 405–411, 1991, Accessed: 00, 2020. [Online]. Available: https://hdl.handle.net/11511/63419.