Paschen lines in M dwarfs chromospheres [Dataset]
The hydrogen Paschen lines are known activity indicators, but studies of them in M dwarfs during quiescence are as rare as their reports in flare studies. This situation is mostly caused by a lack of observations, owing to their location in the near-infrared regime, which is covered by few high-reso...
| Autores: | , , , |
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| Tipo de recurso: | conjunto de datos |
| Fecha de publicación: | 2023 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/365453 |
| Acceso en línea: | http://hdl.handle.net/10261/365453 https://ui.adsabs.harvard.edu/abs/2023A&A...678A...1F https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/678/A1 |
| Access Level: | acceso abierto |
| Palabra clave: | https://cdsarc.cds.unistra.fr/vizier/catstd/ADCkwds.htx Stars, M-type Spectra, infrared |
| Sumario: | The hydrogen Paschen lines are known activity indicators, but studies of them in M dwarfs during quiescence are as rare as their reports in flare studies. This situation is mostly caused by a lack of observations, owing to their location in the near-infrared regime, which is covered by few high-resolution spectrographs. We study the Pa{beta} line, using a sample of 360 M dwarfs observed by the CARMENES spectrograph. Descending the spectral sequence of inactive M stars in quiescence, we find the Pa{beta} line to get shallower until about spectral type M3.5 V, after which a slight re-deepening is observed. Looking at the whole sample, for stars with H{alpha} in absorption, we find a loose anti-correlation between the (median) pseudo-equivalent widths (pEWs) of H{alpha} and Pa{beta} for stars of similar effective temperature. Looking instead at time series of individual stars, we often find correlation between pEW(H{alpha}) and pEW(Pa{beta}) for stars with H{alpha} in emission and an anti-correlation for stars with H{alpha} in absorption. Regarding flaring activity, we report the automatic detection of 35 Paschen line flares in 20 stars. Additionally we found visually six faint Paschen line flares in these stars plus 16 faint Paschen line flares in another 12 stars. In strong flares, Paschen lines can be observed up to Pa 14. Moreover, we find that Paschen line emission is almost always coupled to symmetric H{alpha} line broadening, which we ascribe to Stark broadening, indicating high pressure in the chromosphere. Finally we report a few Pa{beta} line asymmetries for flares that also exhibit strong H{alpha} line asymmetries. |
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