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Peer-reviewedCC BY 4.0The Astrophysical Journal

Frequent X-class Far-ultraviolet Flares from the Young Solar Analog DS Tucanae A

  • Tristen M. Sextro1
  • Kevin France2
  • Vladimir S. Airapetian3,4
  • Grace M. Sweetak1,5,3
  • Randall L. McEntaffer1
  • Kosuke Namekata3,6,7
  • Yuta Notsu2,8
8 affiliations
  1. 1Pennsylvania State University
  2. 2University of Colorado Boulder
  3. 3NASA Goddard Space Flight Center
  4. 4American University
  5. 5Lehigh University
  6. 6The Catholic University of America
  7. 7Kyoto University
  8. 8National Solar Observatory
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Abstract

The young solar analog DS Tuc A (∼45 million yr old, spectral type G6V) serves as an excellent proxy to the Sun during early stages of the Earth’s evolution. The young Sun’s enhanced magnetic activity in the form of X-ray and extreme UV emission, stellar wind, and flares likely affected the magnetospheric and atmospheric environments of early Venus, Earth, and Mars. Studies of DS Tuc A help constrain the evolution of the magnetospheric and atmospheric environments of early Venus, Earth, and Mars and create opportunities to study the impact of flares on the transiting exoplanet, DS Tuc A b. We analyze ∼11 hr of far-ultraviolet (FUV; 1130–1450 Å) observations taken by the Hubble Space Telescope Cosmic Origins Spectrograph during late 2023 and early 2024. We find that DS Tuc A exhibited 26 flares over ∼11.1 hr of observations in the transition region lines Si IV (1394 Å + 1402 Å), with durations ranging from 90 to 960 s and FUV absolute energies ranging from ∼10 ²⁹ to 10 ³¹ erg over the observed bandpass. Si IV flares are accompanied by increases of other chromospheric and transition region lines; however, the strongest Si IV flares show no enhanced coronal emission traced by Fe XXI 1354 Å. We present an analysis of each detected flare, including X-ray and bolometric luminosities scaled from FUV flare energies, electron density measurements for the strongest flares, and the FUV continuum response to flaring. These results provide constraints on the frequency and energetics of flares comparable to X100-class solar flares and FUV-emitting regions in young solar analogs.

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Cite

BibTeXRIS
BibTeX
@article{sextro2026frequent,
  title = {{Frequent X-class Far-ultraviolet Flares from the Young Solar Analog DS Tucanae A}},
  author = {Tristen M. Sextro and Kevin France and Vladimir S. Airapetian and Grace M. Sweetak and Randall L. McEntaffer and Kosuke Namekata and Yuta Notsu},
  journal = {The Astrophysical Journal},
  year = {2026},
  month = oct,
  doi = {10.3847/1538-4357/aea6ae},
  url = {https://iopscience.iop.org/article/10.3847/1538-4357/aea6ae},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Frequent X-class Far-ultraviolet Flares from the Young Solar Analog DS Tucanae A
AU  - Tristen M. Sextro
AU  - Kevin France
AU  - Vladimir S. Airapetian
AU  - Grace M. Sweetak
AU  - Randall L. McEntaffer
AU  - Kosuke Namekata
AU  - Yuta Notsu
PY  - 2026
DA  - 2026/10/26
JO  - The Astrophysical Journal
DO  - 10.3847/1538-4357/aea6ae
UR  - https://iopscience.iop.org/article/10.3847/1538-4357/aea6ae
AB  - The young solar analog DS Tuc A (∼45 million yr old, spectral type G6V) serves as an excellent proxy to the Sun during early stages of the Earth’s evolution. The young Sun’s enhanced magnetic activity in the form of X-ray and extreme UV emission, stellar wind, and flares likely affected the magnetospheric and atmospheric environments of early Venus, Earth, and Mars. Studies of DS Tuc A help constrain the evolution of the magnetospheric and atmospheric environments of early Venus, Earth, and Mars and create opportunities to study the impact of flares on the transiting exoplanet, DS Tuc A b. We analyze ∼11 hr of far-ultraviolet (FUV; 1130–1450 Å) observations taken by the Hubble Space Telescope Cosmic Origins Spectrograph during late 2023 and early 2024. We find that DS Tuc A exhibited 26 flares over ∼11.1 hr of observations in the transition region lines Si IV (1394 Å + 1402 Å), with durations ranging from 90 to 960 s and FUV absolute energies ranging from ∼10 ²⁹ to 10 ³¹ erg over the observed bandpass. Si IV flares are accompanied by increases of other chromospheric and transition region lines; however, the strongest Si IV flares show no enhanced coronal emission traced by Fe XXI 1354 Å. We present an analysis of each detected flare, including X-ray and bolometric luminosities scaled from FUV flare energies, electron density measurements for the strongest flares, and the FUV continuum response to flaring. These results provide constraints on the frequency and energetics of flares comparable to X100-class solar flares and FUV-emitting regions in young solar analogs.
SN  - 0004-637X
SN  - 1538-4357
ER  -