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太陽雑誌会　速報　 2003.04.21 Takako T. Ishii ( 石井 ) Flare Heating in Stellar Coronae

太陽雑誌会　速報　 2003.04.21 Takako T. Ishii ( 石井 ) Flare Heating in Stellar Coronae V.L.Kashyap 1 , J.J.Drake 1 , M.G üdel 2 , and M.Audard 2 1 Harvard-Smithsonian Center for Astrophysics 2 Laboratory for Astrophysics, Paul Scherrer Institute Switzerland ApJ , 580, 1118; 2002 Dec. 1.

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太陽雑誌会　速報　 2003.04.21 Takako T. Ishii ( 石井 ) Flare Heating in Stellar Coronae

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  1. 太陽雑誌会　速報　2003.04.21 Takako T. Ishii (石井) Flare Heating in Stellar Coronae V.L.Kashyap1, J.J.Drake1, M.Güdel2, and M.Audard2 1 Harvard-Smithsonian Center for Astrophysics 2 Laboratory for Astrophysics, Paul Scherrer Institute Switzerland ApJ, 580, 1118; 2002 Dec. 1

  2. Abstract ・Stellar flare Occurrence rate, power-law slope α ・Observed light curve EUVE (Extreme Ultraviolet Explorer) / Deep survey events data 　⇔Modeled light curve + detector characteristics ・Three stars α FK Apr 2.60 ±0.34 V1054 Oph 2.74 ±0.35 AD Leo 2.03 ～ 2.32 Flare component: dominate to the total flux ( > 50 %)

  3. Introduction ・Occurrence rate, power-law slope α ・ α > 2 → small scale flare dominate α < 2 → large scale flare dominate ・Observed energy range (stellar) : E > 1031 erg/s ・This paper, modeling for E > 1029 erg/s compare with observed light curve

  4. Observation

  5. Observation

  6. Observation

  7. Modeling ・Flare occurrence: Assume power-law distribution total flux = flare + background Flare : Poisson process ・Compare the modeled light curve with the observed light curve (＋ detector characteristics) parameter : power-law index α cf. observed light curve → construct dN/dE

  8. Results Observation α=1.8 α=2.1 Model α=2.5 α=3.0

  9. Reliability

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