Stellar models grids White Dwarfs, 0.2 to 8.0 Msun [Dataset]
One of the most reliable means of studying the stellar interior is through the apsidal motion in double line eclipsing binary systems since these systems present errors in masses, radii, and effective temperatures of only a few per cent. On the other hand, the theoretical values of the apsidal motio...
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| Format: | conjunto de datos |
| Publication Date: | 2023 |
| Country: | España |
| Institution: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repository: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/365468 |
| Online Access: | http://hdl.handle.net/10261/365468 https://ui.adsabs.harvard.edu/abs/2023A&A...674A..67C https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/674/A67 |
| Access Level: | Open access |
| Keyword: | https://cdsarc.cds.unistra.fr/vizier/catstd/ADCkwds.htx Models Stars, white dwarf Abundances |
| Summary: | One of the most reliable means of studying the stellar interior is through the apsidal motion in double line eclipsing binary systems since these systems present errors in masses, radii, and effective temperatures of only a few per cent. On the other hand, the theoretical values of the apsidal motion to be compared with the observed values depend on the stellar masses of the components and more strongly on their radii (fifth power). The main objective of this work is to make available grids of evolutionary stellar models that, in addition to the traditional parameters (e.g. age, mass, logg, Teff), also contain the necessary parameters for the theoretical study of apsidal motion and tidal evolution. This information is useful for the study of the apsidal motion in eclipsing binaries and their tidal evolution, and can also be used for the same purpose in exoplanetary systems. |
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