A new oscillating model suggestion for FG Vir

Date

2005-01-01

Author

Kirbiyik, H
Civelek, R
Kiziloglu, N

Metadata

Show full item record

This work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.

Item Usage Stats

66
views

0
downloads

Evolutionary stellar models of FG Vir have been developed theoretically and are compared with earlier observational results. Using the models, we performed calculations to obtain radial and non-radial adiabatic oscillation frequencies. The results show that, if the observational splitting was considered and the observational mode identifications were followed, 1.85M(circle dot) star models with the rotational velocities in the range from 32 to 66 kms(-1) seem to be representative models of FG Vir.

Subject Keywords

Space and Planetary Science, Astronomy and Astrophysics

URI

https://hdl.handle.net/11511/67151

Journal

ASTROPHYSICS AND SPACE SCIENCE

DOI

https://doi.org/10.1007/s10509-005-1085-y

Collections

Department of Physics, Article

Suggestions

OpenMETU
Core

Radial and nonradial oscillations of 44 Tauri Civelek, R; Kiziloglu, N; Kirbiyik, H (American Astronomical Society, 2001-10-01) Evolutionary stellar models of 44 Tauri, a multiperiodic delta Scuti star, have been developed theoretically and compared with earlier observational reports. The models depict 44 Tau at the hydrogen-shell-burning stage, when it is in radiative equilibrium with a very thin surface convective layer. Using the models, we performed calculations to obtain radial and nonradial adiabatic oscillation frequencies, and the equations were treated linearly. The results showed that the radial fundamental (6.899 cycles d...
Modelling the oscillating star V1162 Ori Civelek, R; Kiziloglu, N; Kirbiyik, H (EDP Sciences, 2003-12-01) Evolutionary stellar models of V1162 Ori, with the latest observations of a multiperiodic delta Scuti star, have been calculated theoretically and compared with the observations. Theoretical models representative of the star indicate that it is at an advanced stage of its main-sequence evolution. Calculations have been made for two different masses, 1.80 and 1.82 M-., at different rotational speeds. Rotation was treated as a perturbation and only the first-order effect was considered. The evolutionary model...
Pregalactic-primordial low-mass stars Kızıloğlu, Nilgün Gülşan; Eryurt, Dilhan Ezer (Springer Science and Business Media LLC, 1987-8) The Main-Sequence positions as well as the evolutionary behavior of Population III stars up to an evolution age of 2×1010 yr, taking this time as the age of the Universe, have been investigated in the mass range 0.2 and 0.8M ⊙. While Population III stars with masses greater than 0.3M ⊙ develop a radiative core during the approach to the Main Sequence, stars with masses smaller than 0.3M ⊙ reach the Main Sequence as a wholly convective stars. Population III stars with masses greater than 0.5M ⊙ show a bright...
Main sequence for rotating stars of intermediate mass Eryurtezer, D; Kırbıyık, Hayrettin; Özkara, N (Springer Science and Business Media LLC, 1986) We have investigated the evolutionary behaviour of intermediate mass (2, 3, 4, 5, and 7M ⊙) Population I stars, assuming two different rates of rotation at the threshold of stability. In the first part of the study, stars are assumed to start with a critical rotation (fast rotation model) and to progress to the point of rotational instability. The stars evolve by losing mass and become rotationally unstable before they reach the zero-age Main Sequence. It is argued that multiple star systems might be forme...
Instability of radial oscillations of Wolf-Rayet star models Kırbıyık, Halil (Springer Science and Business Media LLC, 1987) By taking some evolutionary models of an initially 60M ⊙-star, their radial vibrational stabilities have been investigated. These models, evolving with mass loss, are in the advanced stages of their evolution, and burn He in their cores. Calculations have been performed for the first and second harmonics as well as for the fundamental mode; and some of these models were found to be vibrationally unstable in the fundamental mode.

Citation Formats

H. Kirbiyik, R. Civelek, and N. Kiziloglu, “A new oscillating model suggestion for FG Vir,” ASTROPHYSICS AND SPACE SCIENCE, pp. 473–484, 2005, Accessed: 00, 2020. [Online]. Available: https://hdl.handle.net/11511/67151.