Theoretical tidal evolution constants for stellar models from the pre-main sequence to the white dwarf stage: Apsidal motion constants, moment of inertia, and gravitational potential energy
| Autor: | A. Claret |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2023 |
| Předmět: |
Earth and Planetary Astrophysics (astro-ph.EP)
Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science eclipsing [Binaries] interiors [Stars] FOS: Physical sciences evolution [Stars] Astronomy and Astrophysics close [Binaries] Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics - Earth and Planetary Astrophysics |
| Popis: | The Spanish MEC (AYA2015-71718-R and ESP2017-87676-C5-2-R) is gratefully acknowledged for its support during the development of this work. AC also acknowledges financial support from the grant CEX2021-001131-S funded by MCIN/AEI/10.13039/501100011033. This research has made use of the SIMBAD database, operated at the CDS, Strasbourg, France, and of NASA’s Astrophysics Data System Abstract Service Aims. 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, log g, 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. Methods. All models were computed using the MESA package. We consider core overshooting for models with masses ≥ 1.2M⊙. For the amount of core overshooting we adopted a recent relationship for mass × core overshooting. We adopted for the mixing-length parameter αMLT the value 1.84 (the solar-calibrated value). Mass loss was taken into account in two evolutionary phases. The models were followed from the pre-main sequence phase to the white dwarf (WD) stage. Results. The evolutionary models containing age, luminosity, log g, and Teff, as well as the first three harmonics of the internal stellar structure (k2, k3, and k4), the radius of gyration βy, and the dimensionless variable α, related to gravitational potential energy, are presented in 69 tables covering three chemical compositions: [Fe/H] = - 0.50, 0.00, and 0.50. Additional models with different input physics are available. The Spanish MEC AYA2015-71718-R and ESP2017-87676-C5-2-R MCIN/AEI/10.13039/501100011033 CEX2021-001131-S CDS NASA’s Astrophysics Data System Abstract Service |
| Databáze: | OpenAIRE |
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