The Components of Cepheid Systems: The FN Vel System
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arXiv
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| Autori principali: | , , , , , , , , , , |
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| Natura: | Preprint |
| Pubblicazione: |
2024
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| _version_ | 1866914962892390400 |
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| author | Evans, Nancy Remage Kervella, Pierre Kuraszkiewicz, Joanna Günther, H. Moritz Anderson, Richard I. Proffitt, Charles Gallenne, Alexandre Mérand, Antoine Trahin, Boris Viviani, Giordano Shetye, Shreeya |
| author_facet | Evans, Nancy Remage Kervella, Pierre Kuraszkiewicz, Joanna Günther, H. Moritz Anderson, Richard I. Proffitt, Charles Gallenne, Alexandre Mérand, Antoine Trahin, Boris Viviani, Giordano Shetye, Shreeya |
| contents | Cepheid masses continue to be important tests of evolutionary tracks for intermediate mass stars as well as important predictors of their future fate. For systems where the secondary is a B star, {\it Hubble Space Telescope} ultraviolet spectra have been obtained. From these spectra a temperature can be derived, and from this a mass of the companion M$_2$. Once {\it Gaia} DR4 is available, proper motions can be used to determine the inclination of the orbit.
Combining mass of the companion, M$_2$, the mass function from the ground-based orbit of the Cepheid and the inclination produces the mass of the Cepheid, M$_1$. The Cepheid system FN Vel is used here to demonstrate this approach and what limits can be put on the Cepheid mass for inclination between 50 and 130$^o$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_01934 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The Components of Cepheid Systems: The FN Vel System Evans, Nancy Remage Kervella, Pierre Kuraszkiewicz, Joanna Günther, H. Moritz Anderson, Richard I. Proffitt, Charles Gallenne, Alexandre Mérand, Antoine Trahin, Boris Viviani, Giordano Shetye, Shreeya Solar and Stellar Astrophysics Cepheid masses continue to be important tests of evolutionary tracks for intermediate mass stars as well as important predictors of their future fate. For systems where the secondary is a B star, {\it Hubble Space Telescope} ultraviolet spectra have been obtained. From these spectra a temperature can be derived, and from this a mass of the companion M$_2$. Once {\it Gaia} DR4 is available, proper motions can be used to determine the inclination of the orbit. Combining mass of the companion, M$_2$, the mass function from the ground-based orbit of the Cepheid and the inclination produces the mass of the Cepheid, M$_1$. The Cepheid system FN Vel is used here to demonstrate this approach and what limits can be put on the Cepheid mass for inclination between 50 and 130$^o$. |
| title | The Components of Cepheid Systems: The FN Vel System |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2410.01934 |