Stellar Physics with High-Resolution UV Spectropolarimetry
Current burning issues in stellar physics, for both hot and cool stars, concern their magnetism. In hot stars, stable magnetic fields of fossil origin impact their stellar structure and circumstellar environment, with a likely major role in stellar evolution. However, this role is complex and thus p...
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| creator | Morin, Julien Bouret, Jean-Claude Neiner, Coralie Aerts, Conny Bagnulo, Stefano Catala, Claude Charbonnel, Corinne Evans, Chris Fossati, Luca Garcia, Miriam Ana I Gómez de Castro Herrero, Artemio Hussain, Gaitee Kaper, Lex Kochukhov, Oleg Konstantinova-Antova, Renada de Koter, Alex Kraus, Michaela Jiří\K{r}tička Lèbre, Agnes Lueftinger, Theresa Meynet, Georges Petit, Pascal Shore, Steve Solanki, Sami Stelzer, Beate Strugarek, Antoine Vidotto, Aline Vink, Jorick S |
| description | Current burning issues in stellar physics, for both hot and cool stars, concern their magnetism. In hot stars, stable magnetic fields of fossil origin impact their stellar structure and circumstellar environment, with a likely major role in stellar evolution. However, this role is complex and thus poorly understood as of today. It needs to be quantified with high-resolution UV spectropolarimetric measurements. In cool stars, UV spectropolarimetry would provide access to the structure and magnetic field of the very dynamic upper stellar atmosphere, providing key data for new progress to be made on the role of magnetic fields in heating the upper atmospheres, launching stellar winds, and more generally in the interaction of cool stars with their environment (circumstellar disk, planets) along their whole evolution. UV spectropolarimetry is proposed on missions of various sizes and scopes, from POLLUX on the 15-m telescope LUVOIR to the Arago M-size mission dedicated to UV spectropolarimetry. |
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In hot stars, stable magnetic fields of fossil origin impact their stellar structure and circumstellar environment, with a likely major role in stellar evolution. However, this role is complex and thus poorly understood as of today. It needs to be quantified with high-resolution UV spectropolarimetric measurements. In cool stars, UV spectropolarimetry would provide access to the structure and magnetic field of the very dynamic upper stellar atmosphere, providing key data for new progress to be made on the role of magnetic fields in heating the upper atmospheres, launching stellar winds, and more generally in the interaction of cool stars with their environment (circumstellar disk, planets) along their whole evolution. 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| ispartof | arXiv.org, 2019-08 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_proquest_journals_2268874778 |
| source | Freely Accessible Journals |
| subjects | Cool stars High resolution Hot stars Magnetic fields Magnetism Planetary evolution Stellar atmospheres Stellar evolution Stellar magnetic fields Stellar physics Stellar structure Stellar winds |
| title | Stellar Physics with High-Resolution UV Spectropolarimetry |
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