The frequency separations of stellar p-modes
| dc.creator | Yang, W. M. | |
| dc.creator | Bi, S. L. | |
| dc.date | 2007-06-21 | |
| dc.date | 2007-09-03 | |
| dc.date.accessioned | 2026-07-07T08:26:49Z | |
| dc.date.available | 2026-07-07T08:26:49Z | |
| dc.description | Aims. The purpose of this work is to investigate a new frequency separation of stellar p-modes and its characteristics. Methods. Frequency separations are deduced from the asymptotic formula of stellar p-modes. Then, using the theoretical adiabatic frequencies of stellar model, we compute the frequency separations. Results. A new separation $σ_{l-1 l+1}(n)$, which is similar to the scaled small separation $d_{l l+2}(n)/(2l+3)$, is obtained from the asymptotic formula of stellar p-modes. The separations $σ_{l-1 l+1}(n)$ and $d_{l l+2}(n)/(2l+3)$ have the same order. And like the small separation, $σ_{l-1 l+1}(n)$ is mainly sensitive to the conditions in the stellar core. However, with the decrease of the central hydrogen abundance of stars, the $σ_{02}$ and $σ_{13}$ more and more deviate from the scaled small separation. This characteristic could be used to extract the information on the central hydrogen abundance of stars. | |
| dc.description | Accepted for Publication in A&A, 8 pages, 5 figures | |
| dc.identifier | https://arxiv.org/abs/0706.3096 | |
| dc.identifier | http://arxiv.org/abs/0706.3096 | |
| dc.identifier | A&A 472, 571-576 (2007) | |
| dc.identifier | doi:10.1051/0004-6361:20077082 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/137069 | |
| dc.subject | General Relativity and Quantum Cosmology | |
| dc.title | The frequency separations of stellar p-modes | |
| dc.type | text |