SIGMA_GEM
Nano/micro flare heating is a promising explanation for the solar/stellar coronal heating problem. The low-ionized Fe Ka line at 6.4 keV can be a tracer of stellar nano/micro flares. High-energy-resolution spectroscopy is necessary to determine the intensity and photoionization state of the Fe Ka line accurately. The ionization parameter of the Fe Ka line depends on the flare energy scale. We propose a 100 ks Resolve observation of the RS CVn-type star Sigma Gem to reproduce the flare frequency distribution of stellar nano/micro flares and investigate whether the temperature of the Sigma Gem corona can be explained by the sum of the energies of them. We also use Xtend to determine the temperature of the quiescent corona of Sigma Gem during the Resolve observation.
obsid = 202063010 / Unique Observation/Sequence Number
object = SIGMA_GEM / Object name
pi_name = INOUE SHUN / Proposal Principal Investigator Name
ra = 115.826825287381 / Right Ascension (Pointing Position) (deg)
dec = 28.8839766700562 / Declination (Pointing Position) (deg)
roll_angle = 100.001375303249 / Roll Angle (deg)
start_time = 2025-11-06T22:19:04 / Start Time of the Observation
stop_time = 2025-11-09T08:52:04 / Stop Time of the Observation
exposure = 109075.60868 / Effective Total Observation Exposure (s)
public_date= 2026-11-15 / Public Date