Rotationally Driven Ultraviolet Emission of Red Giant Stars. II. Metallicity, Activity, Binarity, and Subsubgiants
Red-giant-branch (RGB) stars are overwhelmingly observed to rotate very slowly compared to main-sequence stars, but a few percent of them show rapid rotation and high activity, often as a result of tidal synchonization or other angular momentum transfer events. In this paper we build upon previous w...
I tiakina i:
| Ngā kaituhi matua: | , , , , |
|---|---|
| Hōputu: | Artigo |
| Reo: | Inglês |
| I whakaputaina: |
IOP Publishing
2025-01-01
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| Rangatū: | The Astronomical Journal |
| Ngā marau: | |
| Urunga tuihono: | https://doi.org/10.3847/1538-3881/adc92a |
| Ngā Tūtohu: |
Kāore He Tūtohu, Me noho koe te mea tuatahi ki te tūtohu i tēnei pūkete!
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