The physics of flares in young stellar objects

Details The physics of flares in young stellar objects The physics of flares in young stellar objects

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006cxo..prop.2507m&link_type=abstract

Chandra Proposal ID #08108279

Physics

Chandra Proposal Id #08108279

Scientific paper

Flares are the most extreme manifestation of stellar activity. Magnetic reconnection produces fast electrons that hit the stellar surface to produce chromospheric material evaporation. Non-thermal heating shows up as impulsive flares in optical and hard X-rays, and evaporation as longer soft X-ray flares. Multi-band observations covering thermal and non-thermal components are essential to understand the physics of flaring. The CoRoT space telescope will continuously observe the star forming region NGC2264 for 20 days in March 2008 in the optical with unprecedented photometric precision and with a temporal resolution of 10s of sec, ideal for the detection of impulsive events. We ask for two 100ksec observations in the two most populated cluster regions during the CoRoT observation to simultaneously study the non-thermal (CoRoT) and the thermal (Chandra) components of flares. 100s of flaring sources have already been detected in a single ACIS field in NGC2264 (Flaccomio et al. 2006).

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