دورية أكاديمية
The CARMENES search for exoplanets around M dwarfs: The He » i infrared triplet lines in PHOENIX models of M 2-3 v stars
| العنوان: | The CARMENES search for exoplanets around M dwarfs: The He » i infrared triplet lines in PHOENIX models of M 2-3 v stars |
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| المؤلفون: | Hintz, D., Fuhrmeister, B., Czesla, S., Schmitt, Jürgen H. M. M., Schweitzer, A., Nagel, E., Johnson, E.N., Caballero, J. A., Zechmeister, M., Jeffers, S.V., Reiners, A., Amado, Pedro J., Quirrenbach, A., Anglada-Escudé, Guillem, Bauer, FF, Béjar, V.J.S., Cortés-Contreras, M., Dreizler, S., Galadí-Enriquez, D., Guenther, E.W., Hauschildt, P. H., Kaminski, Adrian, Kürster, M., Lafarga, M., López del Fresno, M., Montes, D., Morales, J.C. |
| المساهمون: | Ribas, Ignasi |
| بيانات النشر: | Springer |
| سنة النشر: | 2020 |
| المجموعة: | Digital.CSIC (Consejo Superior de Investigaciones Científicas / Spanish National Research Council) |
| الوصف: | The He » I infrared (IR) line at a vacuum wavelength of 10 833 Å is a diagnostic for the investigation of atmospheres of stars and planets orbiting them. For the first time, we study the behavior of the He » I IR line in a set of chromospheric models for M-dwarf stars, whose much denser chromospheres may favor collisions for the level population over photoionization and recombination, which are believed to be dominant in solar-type stars. For this purpose, we use published PHOENIX models for stars of spectral types M2 V and M3 V and also compute new series of models with different levels of activity following an ansatz developed for the case of the Sun. We perform a detailed analysis of the behavior of the He I IR line within these models. We evaluate the line in relation to other chromospheric lines and also the influence of the extreme ultraviolet (EUV) radiation field. The analysis of the He » I IR line strengths as a function of the respective EUV radiation field strengths suggests that the mechanism of photoionization and recombination is necessary to form the line for inactive models, while collisions start to play a role in our most active models. Moreover, the published model set, which is optimized in the ranges of the Na » I D2, Hα, and the bluest Ca » II IR triplet line, gives an adequate prediction of the He » I IR line for most stars of the stellar sample. Because especially the most inactive stars with weak He » I IR lines are fit worst by our models, it seems that our assumption of a 100% filling factor of a single inactive component no longer holds for these stars. ; With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737) |
| نوع الوثيقة: | article in journal/newspaper |
| اللغة: | unknown |
| تدمد: | 1432-0746 |
| العلاقة: | http://dx.doi.org/10.1051/0004-6361/202037596Test; Sí; Astronomy and Astrophysics 638 (2020); http://hdl.handle.net/10261/234359Test |
| DOI: | 10.1051/0004-6361/202037596 |
| الإتاحة: | https://doi.org/10.1051/0004-6361/202037596Test http://hdl.handle.net/10261/234359Test |
| حقوق: | none |
| رقم الانضمام: | edsbas.509F02EA |
| قاعدة البيانات: | BASE |
Full Text Finder | تدمد: | 14320746 |
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| DOI: | 10.1051/0004-6361/202037596 |