M dwarfs quasi-periodic pulsations at a time resolution of 1 s
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arXiv
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| Hauptverfasser: | , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866915057159372800 |
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| author | Panferov, Alexander Beskin, Grigory Karpov, Sergey Maryeva, Olga |
| author_facet | Panferov, Alexander Beskin, Grigory Karpov, Sergey Maryeva, Olga |
| contents | Quasi-periodic pulsations (QPPs) of Sun and stars are challenging for stellar flare models. The white light stellar QPPs in the periodicity region of tens of second are unexplored yet. On the basis of observations with the 6-m telescope BTA in U-band of flaring dM-stars EV Lac, Wolf 359, Wolf 424, V577 Mon and UV Ceti we found 13 new QPPs. This composes 30% occurrence among 44 worked flares. These QPPs were found to have periods ranging from 6 to 107 seconds and were detected using both Fourier transform and empirical mode decomposition methods. The observed QPPs were categorized by the evolution of their oscillation envelope and fractional flux amplitudes. There are shown the statistically significant correlations of the QPP period with the duration, the equivalent duration and the amplitude of a flare, and the correlation between the QPP amplitude and flare amplitude. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2412_07580 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | M dwarfs quasi-periodic pulsations at a time resolution of 1 s Panferov, Alexander Beskin, Grigory Karpov, Sergey Maryeva, Olga Solar and Stellar Astrophysics Quasi-periodic pulsations (QPPs) of Sun and stars are challenging for stellar flare models. The white light stellar QPPs in the periodicity region of tens of second are unexplored yet. On the basis of observations with the 6-m telescope BTA in U-band of flaring dM-stars EV Lac, Wolf 359, Wolf 424, V577 Mon and UV Ceti we found 13 new QPPs. This composes 30% occurrence among 44 worked flares. These QPPs were found to have periods ranging from 6 to 107 seconds and were detected using both Fourier transform and empirical mode decomposition methods. The observed QPPs were categorized by the evolution of their oscillation envelope and fractional flux amplitudes. There are shown the statistically significant correlations of the QPP period with the duration, the equivalent duration and the amplitude of a flare, and the correlation between the QPP amplitude and flare amplitude. |
| title | M dwarfs quasi-periodic pulsations at a time resolution of 1 s |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2412.07580 |