Early optical follow-up of the nearby active star DG CVn during its 2014 superflare

Abstract

DG CVn is a binary system in which one of the components is an M type dwarf ultra fast rotator, only three of which are known in the solar neighborhood. Observations of DG CVn by the Swift satellite and several ground-based observatories during its super-flare event on 2014 allowed us to perform a complete hard X-ray - optical follow-up of a super-flare from the red-dwarf star. The observations support the fact that the super-flare can be explained by the presence of (a) large active region(s) on the surface of the star. Such activity is similar to the most extreme solar flaring events. This points towards a plausible extrapolation between the behaviour from the most active red-dwarf stars and the processes occurring in the Sun.

arXiv commentAccepted for publication in MNRAS (10/07/15). 9 pages (5 figures and 2 tables)

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• A Very Bright, Very Hot, and Very Long Flaring Event from the M Dwarf Binary System DG CVn
• Time resolved spectroscopic observations of an M-dwarf flare star EV Lacertae during a flare
• Blasts from the Past: Supernova Shock Breakouts among X-Ray Transients in the XMM-Newton Archive
• On the expected $\gamma$-ray emission from nearby flaring stars
• Fermi/LAT detection of a transient gamma-ray flare in the vicinity of the binary star DG CVn
• A Seven-Day Multi-Wavelength Flare Campaign on AU Mic III: Quiescent and Flaring Properties of the X-ray Spectra and Chromospheric lines
• Time Domain Astronomy with the THESEUS Satellite