Speaker
Description
Gamma-ray emission from stellar activity, usually generated from relativistic particles, plays an important role in the space weather and habitability of exoplanets. Young dwarf stars of K-type and later are far more magnetically active than the Sun, yet only one other isolated main sequence star (TVLM 513-46546) apart from the Sun is detected in gamma-rays. Stacking surveys of radio, optical and X-ray flares of K-type and later dwarf stars using Fermi-LAT data during the flares placed a sensitive upper limit of their gamma-ray emission. The gamma-ray emission from stellar flares likely originates from the decay of neutral pions. They are generated by relativistic protons interacting within the stellar atmosphere. If the protons are accelerated to TeV energies, this emission mechanism might be able to produce TeV gamma-rays. This work aims to verify the detectability of stellar flares in CTA using existing observations from Fermi-LAT. Furthermore, it will serve as a guideline to determine which stars, based on their distance and flare events, can be detected in CTA.
