A magnetic tertiary in the most massive compact triple-star system
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866913846615080960 |
|---|---|
| author | Hubrig, S. Vigna-Gómez, A. Järvinen, S. P. Schöller, M. Ilyin, I. |
| author_facet | Hubrig, S. Vigna-Gómez, A. Järvinen, S. P. Schöller, M. Ilyin, I. |
| contents | The system TIC 470710327 is comprised of three main-sequence OB stars, with an inner compact 1.10 d eclipsing binary and a non-eclipsing tertiary on a 52.04 d orbit. With the tertiary mass of 14.5-16 $M_{\odot}$ and both components in the inner eclipsing binary with individual masses of 6--7 and 5.5-6.3 $M_{\odot}$, it is currently the most massive compact system known. The formation scenario of such a compact triple is uncertain. It has been suggested that `2 + 2' quadruple dynamics can lead to a stellar merger in the initially more massive binary and finally result in a highly magnetised tertiary. Our study confirms the presence of a kG-order magnetic field in the tertiary and the slow rotation typical for massive magnetic stars. We conclude that finding massive merger candidates by studies of dynamics in compact, multiple-star systems is an efficient way to understand the evolution of massive stellar multiplicity and the generation of magnetic fields. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_12852 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A magnetic tertiary in the most massive compact triple-star system Hubrig, S. Vigna-Gómez, A. Järvinen, S. P. Schöller, M. Ilyin, I. Solar and Stellar Astrophysics High Energy Astrophysical Phenomena The system TIC 470710327 is comprised of three main-sequence OB stars, with an inner compact 1.10 d eclipsing binary and a non-eclipsing tertiary on a 52.04 d orbit. With the tertiary mass of 14.5-16 $M_{\odot}$ and both components in the inner eclipsing binary with individual masses of 6--7 and 5.5-6.3 $M_{\odot}$, it is currently the most massive compact system known. The formation scenario of such a compact triple is uncertain. It has been suggested that `2 + 2' quadruple dynamics can lead to a stellar merger in the initially more massive binary and finally result in a highly magnetised tertiary. Our study confirms the presence of a kG-order magnetic field in the tertiary and the slow rotation typical for massive magnetic stars. We conclude that finding massive merger candidates by studies of dynamics in compact, multiple-star systems is an efficient way to understand the evolution of massive stellar multiplicity and the generation of magnetic fields. |
| title | A magnetic tertiary in the most massive compact triple-star system |
| topic | Solar and Stellar Astrophysics High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2505.12852 |