Magnetic activity cycles in the exoplanet host star ε eridani
The active K2 dwarf ε Eri has been extensively characterized both as a young solar analog and more recently as an exoplanet host star. As one of the nearest and brightest stars in the sky, it provides an unparalleled opportunity to constrain stellar dynamo theory beyond the Sun. We confirm and docum...
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2013
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| Acceso en línea: | https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_20418205_v763_n2_p_Metcalfe http://hdl.handle.net/20.500.12110/paper_20418205_v763_n2_p_Metcalfe |
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paper:paper_20418205_v763_n2_p_Metcalfe2023-06-08T16:33:16Z Magnetic activity cycles in the exoplanet host star ε eridani Buccino, Andrea Paola Mauas, Pablo J.D. Petrucci, Romina Paola stars: activity stars: chromospheres stars: individual (HD 22049) surveys The active K2 dwarf ε Eri has been extensively characterized both as a young solar analog and more recently as an exoplanet host star. As one of the nearest and brightest stars in the sky, it provides an unparalleled opportunity to constrain stellar dynamo theory beyond the Sun. We confirm and document the 3-year magnetic activity cycle in ε Eri originally reported by Hatzes and coworkers, and we examine the archival data from previous observations spanning 45 years. The data show coexisting 3-year and 13-year periods leading into a broad activity minimum that resembles a Maunder minimum-like state, followed by the resurgence of a coherent 3-year cycle. The nearly continuous activity record suggests the simultaneous operation of two stellar dynamos with cycle periods of 2.95 ± 0.03 years and 12.7 ± 0.3 years, which, by analogy with the solar case, suggests a revised identification of the dynamo mechanisms that are responsible for the so-called "active" and "inactive" sequences as proposed by Böhm-Vitense. Finally, based on the observed properties of ε Eri, we argue that the rotational history of the Sun is what makes it an outlier in the context of magnetic cycles observed in other stars (as also suggested by its Li depletion), and that a Jovian-mass companion cannot be the universal explanation for the solar peculiarities. © 2013. The American Astronomical Society. All rights reserved.. Fil:Buccino, A.P. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Mauas, P.J.D. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Petrucci, R. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2013 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_20418205_v763_n2_p_Metcalfe http://hdl.handle.net/20.500.12110/paper_20418205_v763_n2_p_Metcalfe |
| institution |
Universidad de Buenos Aires |
| institution_str |
I-28 |
| repository_str |
R-134 |
| collection |
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) |
| topic |
stars: activity stars: chromospheres stars: individual (HD 22049) surveys |
| spellingShingle |
stars: activity stars: chromospheres stars: individual (HD 22049) surveys Buccino, Andrea Paola Mauas, Pablo J.D. Petrucci, Romina Paola Magnetic activity cycles in the exoplanet host star ε eridani |
| topic_facet |
stars: activity stars: chromospheres stars: individual (HD 22049) surveys |
| description |
The active K2 dwarf ε Eri has been extensively characterized both as a young solar analog and more recently as an exoplanet host star. As one of the nearest and brightest stars in the sky, it provides an unparalleled opportunity to constrain stellar dynamo theory beyond the Sun. We confirm and document the 3-year magnetic activity cycle in ε Eri originally reported by Hatzes and coworkers, and we examine the archival data from previous observations spanning 45 years. The data show coexisting 3-year and 13-year periods leading into a broad activity minimum that resembles a Maunder minimum-like state, followed by the resurgence of a coherent 3-year cycle. The nearly continuous activity record suggests the simultaneous operation of two stellar dynamos with cycle periods of 2.95 ± 0.03 years and 12.7 ± 0.3 years, which, by analogy with the solar case, suggests a revised identification of the dynamo mechanisms that are responsible for the so-called "active" and "inactive" sequences as proposed by Böhm-Vitense. Finally, based on the observed properties of ε Eri, we argue that the rotational history of the Sun is what makes it an outlier in the context of magnetic cycles observed in other stars (as also suggested by its Li depletion), and that a Jovian-mass companion cannot be the universal explanation for the solar peculiarities. © 2013. The American Astronomical Society. All rights reserved.. |
| author |
Buccino, Andrea Paola Mauas, Pablo J.D. Petrucci, Romina Paola |
| author_facet |
Buccino, Andrea Paola Mauas, Pablo J.D. Petrucci, Romina Paola |
| author_sort |
Buccino, Andrea Paola |
| title |
Magnetic activity cycles in the exoplanet host star ε eridani |
| title_short |
Magnetic activity cycles in the exoplanet host star ε eridani |
| title_full |
Magnetic activity cycles in the exoplanet host star ε eridani |
| title_fullStr |
Magnetic activity cycles in the exoplanet host star ε eridani |
| title_full_unstemmed |
Magnetic activity cycles in the exoplanet host star ε eridani |
| title_sort |
magnetic activity cycles in the exoplanet host star ε eridani |
| publishDate |
2013 |
| url |
https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_20418205_v763_n2_p_Metcalfe http://hdl.handle.net/20.500.12110/paper_20418205_v763_n2_p_Metcalfe |
| work_keys_str_mv |
AT buccinoandreapaola magneticactivitycyclesintheexoplanethoststareeridani AT mauaspablojd magneticactivitycyclesintheexoplanethoststareeridani AT petruccirominapaola magneticactivitycyclesintheexoplanethoststareeridani |
| _version_ |
1768544524753174528 |