Colliding Magnetospheres in The Young High-Eccentricity Binary DQ Tau: Conclusions
by Magnetosphere: Maintaining Habitability on EarthMay 10th, 2024
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In this paper, researchers conducted NuSTAR, Swift, and Chandra observations on the DQ Tau high-eccentricity binary system to confirm the presence of X-ray super-flares.
This paper is available on arxiv under CC 4.0 license.
Authors:
(1) Konstantin V. Getman, Department of Astronomy & Astrophysics, Pennsylvania State University;
(2) Agnes Kospal, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, E¨otv¨os Lor´and Research Network (ELKH), MTA Centre of Excellence, Max Planck Institute for Astronomy, and ELTE E¨otv¨os Lor´and University, Institute of Physics;
(3) Nicole Arulanantham, Space Telescope Science Institute;
(4) Dmitry A. Semenov, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences;
(5) Grigorii V. Smirnov-Pinchukov, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences;
(6) Sierk E. van Terwisga, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences.
Table of Links
- Abstract and Intro
- X-ray Observations and Data Extraction
- Flare Analyses
- Comparison with X-ray Flares from Young Stars
- Discussion
- Conclusions
- Acknowledgments and References
6. CONCLUSIONS
Drawing upon recent observations conducted during a single orbit of DQ Tau in July-August 2022, which utilized NuSTAR, Swift, and Chandra telescopes (§ 2), alongside previously gathered X-ray and mm-band data from multiple periastrons of DQ Tau (Salter et al. 2010; Getman et al. 2011, 2022b), our study embarks on an extensive analysis to compute the energetic characteristics of X-ray/NUV/optical flares within DQ Tau (§ 3).
Serendipitously, we discovered X-ray super-flares outside of periastron, potentially related to interacting magnetospheres (§ 5.1.2).
The absence of evidence for long-term variability in the baseline X-ray emission of ∼ 1 Myr old DQ Tau is consistent with the understanding that younger stars typically exhibit larger active regions and more extensive X-ray coronal structures. This may contribute to the reduction of observable magnetic dynamo cycling (§ 5.3).
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