1 太陽雑誌会速報 2004.05.24 T.T.Ishii The Astrophysical Journal, 607:L131–L134, 2004 June 1 NEAR-INFRARED OBSERVATIONS AT 1.56 MICRONS OF THE 2003 OCTOBER 29.

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太陽雑誌会速報2004.05.24

T.T.IshiiThe Astrophysical Journal, 607:L131–L134, 2004 June 1

NEAR-INFRARED OBSERVATIONS AT 1.56 MICRONS OF THE 2003 OCTOBER 29 X10 WHITE-LIGHT FLARE

Yan Xu,1 Wenda Cao,1,2 Chang Liu,1 Guo Yang,1 Jiong Qiu,1,2 Ju Jing,1 Carsten Denker,1,2 and Haimin Wang1,2

Received 2004 March 12; accepted 2004 April 22; published 2004 May 4

1 Center for Solar-Terrestrial Research, New Jersey Institute of Technology,

2 Big Bear Solar Observatory

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Near-infrared (NIR/1.6m) image of the X10 flare

Dunn Solar Telescope at Sac Peakwith high-order AO(adaptive optics)

FOV: 91”×91”CCD: 1024×1024→0.0089”/pixel

2003-Oct-2920:42 UTFlare onset: 20:37peak: 20:49

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NIR time sequence of the X10 flare with RHESSI HXR contour from 20:40 to 20:47 (1 image / 1 min.)

Blue: RHESSI HXR contour (50-100 keV channel)Red: local NIR intensity maxima (flare ribbons in NIR)

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Temporal evolution of the NIR flare ribbonson SOHO/MDI longitudinal magetogram

Separation speed: 38 km/s within weak field (700 G), 19 km/s (1400G)

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Forbes & Priest (1984) and Forbes & Lin (2000)Ec : electric field strength along the current sheet vt : ribbon separation speedBn: longitudinal magnetic field (near disk center)

⇒ Ec= 45 V/cm (much larger than previous results)

Intensity enhancement (18-25 % to quiet-Sun in NIR)→ temperature perturbation Wang et al. (1998)

→ radiative loss

⇒ 1031 ergs within 8 minutes

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The Astrophysical Journal, 607:L59–L62, 2004 May 20

ON THE ORIGIN OF SOLAR FACULAE

C. U. Keller,1,2 M. Schüssler,1 A. Vögler,1

and V. Zakharov1

Received 2004 March 9; accepted 2004 April 5; published 2004 April 22

1 Max-Planck-Institut für Aeronomie

2 On sabbatical leave from the National Solar Observatory

太陽雑誌会速報2004.05.24

T.T.Ishii

7http://www.linmpi.mpg.de/~msch/Thesis_Voegler.pdf

ab initio three-dimensional simulations of nongray radiative magnetoconvectionin the solar surface layers with the MURaM code

(Max-Planck Institute for Aeronomy and University of Chicago Radiative Magnetohydrodynamics code)

Numerical MHD simulations

(100×288×288 grid points)

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ObservationLites et al. 2004LaPalma1m Swedish Solar Telescope

SimulationB=400G = 60 deg.(viewing angle)

Upward = Limb-ward

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Bright wall modelContinuum intensity &Slices of physical quantities(dash line: continuum level)

→Limb-ward