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Peer-reviewedCC BY 4.0The Astrophysical Journal

Frequent Optical Flares in an M-type Detached Eclipsing Binary TIC 349005337

  • Xiao Zhou1
  • Liying Zhu1
  • Wei Hu2
  • Gil Nachmani3
  • Jia Zhang4
  • Mikhail Yu. Kovalev1,5
  • Ergang Zhao1
5 affiliations
  1. 1Chinese Academy of Sciences
  2. 2Lishui University
  3. 3Tel Aviv University
  4. 4Leshan Normal University
  5. 5Yunnan Key Laboratory
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Abstract

A comprehensive photometric and spectroscopic analysis of TIC 349005337, a highly active M-type detached eclipsing binary with an orbital period of 2.6079133 days, is presented utilizing high-cadence and long-term monitoring photometry from the Transiting Exoplanet Survey Satellite (TESS) and medium-resolution spectroscopy from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST). By integrating radial velocity curves with light curves, we determined the fundamental physical parameters for both components. The system consists of an M-dwarf primary ( M ₁ = 0.517 ± 0.009 M ⊙ , R ₁ = 0.518 ± 0.003 R ⊙ ) and a fully convective secondary ( M ₂ = 0.298 ± 0.004 M ⊙ , R ₂ = 0.357 ± 0.003 R ⊙ ). A total of 12 high-energy stellar flares, with the most energetic event reaching 3.87 × 10 ³⁴ erg, is identified, confirming the system is in a state of magnetic hyperactivity. The frequent superflares suggest that intense magnetic activity and significant starspot coverage play a dominant role in altering the stellar atmospheric structure. As the secondary component falls below the fully convective boundary, these energetic flares provide critical empirical constraints for distributed dynamo models in the low-mass regime. Our results highlight TIC 349005337 as an ideal laboratory for investigating the interplay between binary dynamics, magnetic reconnection, and the resulting impact on the atmospheric stability of potential orbiting exoplanets.

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Cite

BibTeXRIS
BibTeX
@article{zhou2026frequent,
  title = {{Frequent Optical Flares in an M-type Detached Eclipsing Binary TIC 349005337}},
  author = {Xiao Zhou and Liying Zhu and Wei Hu and Gil Nachmani and Jia Zhang and Mikhail Yu. Kovalev and Ergang Zhao},
  journal = {The Astrophysical Journal},
  year = {2026},
  month = nov,
  doi = {10.3847/1538-4357/aeacc3},
  url = {https://iopscience.iop.org/article/10.3847/1538-4357/aeacc3},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Frequent Optical Flares in an M-type Detached Eclipsing Binary TIC 349005337
AU  - Xiao Zhou
AU  - Liying Zhu
AU  - Wei Hu
AU  - Gil Nachmani
AU  - Jia Zhang
AU  - Mikhail Yu. Kovalev
AU  - Ergang Zhao
PY  - 2026
DA  - 2026/11/02
JO  - The Astrophysical Journal
DO  - 10.3847/1538-4357/aeacc3
UR  - https://iopscience.iop.org/article/10.3847/1538-4357/aeacc3
AB  - A comprehensive photometric and spectroscopic analysis of TIC 349005337, a highly active M-type detached eclipsing binary with an orbital period of 2.6079133 days, is presented utilizing high-cadence and long-term monitoring photometry from the Transiting Exoplanet Survey Satellite (TESS) and medium-resolution spectroscopy from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST). By integrating radial velocity curves with light curves, we determined the fundamental physical parameters for both components. The system consists of an M-dwarf primary ( M ₁ = 0.517 ± 0.009 M ⊙ , R ₁ = 0.518 ± 0.003 R ⊙ ) and a fully convective secondary ( M ₂ = 0.298 ± 0.004 M ⊙ , R ₂ = 0.357 ± 0.003 R ⊙ ). A total of 12 high-energy stellar flares, with the most energetic event reaching 3.87 × 10 ³⁴ erg, is identified, confirming the system is in a state of magnetic hyperactivity. The frequent superflares suggest that intense magnetic activity and significant starspot coverage play a dominant role in altering the stellar atmospheric structure. As the secondary component falls below the fully convective boundary, these energetic flares provide critical empirical constraints for distributed dynamo models in the low-mass regime. Our results highlight TIC 349005337 as an ideal laboratory for investigating the interplay between binary dynamics, magnetic reconnection, and the resulting impact on the atmospheric stability of potential orbiting exoplanets.
SN  - 1538-4357
SN  - 0004-637X
ER  -