TESS Science Conference 2
Published July 23, 2021 | Version v1
Poster Open

Blue asymmetries in Balmer lines during mid M dwarf flares

Creators

  • 1. CU Boulder / LASP / NSO / Tokyo Tech
  • 2. CU Boulder / LASP / NSO
  • 3. NAOJ
  • 4. University of Hyogo
  • 5. RIKEN
  • 6. NASA/GSFC, UMBC
  • 7. University of Washington
  • 8. Kyoto University

Contributors

  • 1. Planetary Science Institute

Description

Flares are releases of magnetic energy in the stellar atmosphere, and they have strong emissions from radio to X-rays. During some M dwarf flares, chromospheric line profiles show blue asymmetries, although red asymmetries are more commonly observed in solar flares. Similar enhancements of the blue wings of Balmer lines may provide clues for investigating the early phases of stellar coronal mass ejections (CMEs), but this is still controversial. Thus, we need more observations to understand the relationship between mass ejections and flares. We have conducted simultaneous spectroscopic and photometric observations of mid M dwarf flare stars using APO 3.5m/ARCES, SMARTS1.5m/CHIRON, TESS, and etc. During 34 night observations, we detected 48 flares in Balmer lines (e.g. Hα). At least 7 flares show clear blue asymmetries. Blue asymmetry durations are different among the 7 events (20min ~ 2hr). These results suggest upward flows of chromospheric plasma during flare events. By assuming that the blue asymmetries were caused by prominence eruptions, we estimated the mass and kinetic energy. The estimated masses are comparable to expectations from the empirical relation between the flare X-ray energy and mass of solar CMEs.

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Additional details

References

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