太陽雑誌会 速報 
This presentation is the property of its rightful owner.
Sponsored Links
1 / 9

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


  • 84 Views
  • Uploaded on
  • Presentation posted in: General

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.

Download Presentation

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

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Presentation Transcript


2003 04 21 takako t ishii 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.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


2003 04 21 takako t ishii flare heating in stellar coronae

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 Leo2.03 ~ 2.32

Flare component: dominate to the total flux ( > 50 %)


2003 04 21 takako t ishii flare heating in stellar coronae

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


2003 04 21 takako t ishii flare heating in stellar coronae

Observation


2003 04 21 takako t ishii flare heating in stellar coronae

Observation


2003 04 21 takako t ishii flare heating in stellar coronae

Observation


2003 04 21 takako t ishii flare heating in stellar coronae

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


2003 04 21 takako t ishii flare heating in stellar coronae

Results

Observation

α=1.8

α=2.1

Model

α=2.5

α=3.0


2003 04 21 takako t ishii flare heating in stellar coronae

Reliability


  • Login