Rediscussion of eclipsing binaries. Paper XXII. The B-type system MU Cassiopeiae
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arXiv
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| Formato: | Preprint |
| Publicado: |
2024
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| _version_ | 1866916461451149312 |
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| author | Southworth, John |
| author_facet | Southworth, John |
| contents | MU Cas is a detached eclipsing binary containing two B5 V stars in an orbit of period 9.653 d and eccentricity 0.192, which has been observed in seven sectors using the Transiting Exoplanet Survey Satellite (TESS). We use these new light curves together with published spectroscopic results to measure the physical properties of the component stars, finding masses of 4.67 +/- 0.09 Msun and 4.59 +/- 0.08 Msun, and radii of 4.12 +/- 0.04 Rsun and 3.65 +/- 0.05 Rsun. These values agree with previous results save for a change in which of the two stars is designated the primary component. The measured distance to the system, 1814 +/- 37 pc, is 1.8$σ$ shorter than the distance from the Gaia DR3 parallax. A detailed spectroscopic analysis of the system is needed to obtain improved temperature and radial velocity measurements for the component stars; a precise spectroscopic light ratio is also required for better measurement of the stellar radii. MU Cas matches the predictions of theoretical stellar evolutionary models for a solar chemical composition and an age of 87 +/- 5 Myr. No evidence for pulsations was found in the light curves. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_23011 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Rediscussion of eclipsing binaries. Paper XXII. The B-type system MU Cassiopeiae Southworth, John Solar and Stellar Astrophysics MU Cas is a detached eclipsing binary containing two B5 V stars in an orbit of period 9.653 d and eccentricity 0.192, which has been observed in seven sectors using the Transiting Exoplanet Survey Satellite (TESS). We use these new light curves together with published spectroscopic results to measure the physical properties of the component stars, finding masses of 4.67 +/- 0.09 Msun and 4.59 +/- 0.08 Msun, and radii of 4.12 +/- 0.04 Rsun and 3.65 +/- 0.05 Rsun. These values agree with previous results save for a change in which of the two stars is designated the primary component. The measured distance to the system, 1814 +/- 37 pc, is 1.8$σ$ shorter than the distance from the Gaia DR3 parallax. A detailed spectroscopic analysis of the system is needed to obtain improved temperature and radial velocity measurements for the component stars; a precise spectroscopic light ratio is also required for better measurement of the stellar radii. MU Cas matches the predictions of theoretical stellar evolutionary models for a solar chemical composition and an age of 87 +/- 5 Myr. No evidence for pulsations was found in the light curves. |
| title | Rediscussion of eclipsing binaries. Paper XXII. The B-type system MU Cassiopeiae |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2410.23011 |