Abstract:
Super flares emitted by the young m-dwarf star have long been considered a product of thermal emission. G227-22 is a mid-aged, pre-Main Sequence M dwarf star observed from the second year through the sixth year of science observation of the Transiting Exoplanet Survey Satellite (TESS). As the star is located near the celestial north pole, providing us with a continuous set of data from both TESS and CARMENES, we get to study the flare activity of the star, spanning around four years of observation. In this paper, we measure the flare activity of the star and study a total number of 1962 flares from sector 14 to sector 76 of TESS science observation, along with the data from our observation in Ariel University Telescope and Wise Observatory. We collected data using two different filters to study the star's flare in different parts of the spectrum. We propose a combined analysis of all to ascertain the eruption on the surface of the star, which is not a mere consequence of black-body radiation but an offshoot of line spectrum emissions.
Description:
The conventional notion of considering the M dwarf superflares as a mere product of thermal emission does not fit the new research findings. A pre-main sequence star named G227-22 lies closer to the celestial north pole, providing us with a continuous set of observational data from both TESS and CARMENES, proving the above to form a hypothesis. From the study of the star’s flare activity in the period of two weeks, along with the six years of data from TESS, we are able to conclude that the eruption on the star’s surface can not just considered to be a black-body radiation but the line spectrum emissions.
