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NBYM04 Introduction

NBYM04 Introduction. “Symposium on Nobeyama Radioheliograph” 1990 November 26-28 @ NRO “Kofu symposium – New look at the Sun with emphasis on advanced Observations of coronal dynamics and flares” 1994 September 6-10 @ Kofu “Solar physics with radio observations”

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NBYM04 Introduction

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  1. NBYM04 Introduction • “Symposium on Nobeyama Radioheliograph” • 1990 November 26-28 @ NRO • “Kofu symposium – New look at the Sun with emphasis on advanced Observations of coronal dynamics and flares” • 1994 September 6-10 @ Kofu • “Solar physics with radio observations” • 1998 October 27 – 30 @ Kiyosato • “Solar physics with the Nobeyama Radioheliograph” － 2004 October 26 – 29 @ Kiyosato

  2. Nobeyama Radioheliograph • Proposal: early 1980s (Prof. Haruo Tanaka, 1985) • Reorganization: NAOJ (1988) Merger of Toyokawa and Nobeyama groups • Construction: 1990 – 1991 (Prof. Keizo Kai, 1991) • YOHKOH launched 1991 August • Routine observation 1992 June/July • Dual frequency 1995 • Another reorganization NSRO/NAO/NINS(2004)

  3. Main target • Particle acceleration mechanisms in solar flares? • No answer yet • Existing MHD solar flare theory does not include particle acceleration • Observed features do not fit to the existing theory • Two- or multi-loop configuration • Non-thermal loop (no evaporation from footpoints) • Flare associated oscillations

  4. Flare geometry found by NoRH

  5. Nonthermal electron injection(filling process of nonthermal loop with light speed) Earth size

  6. Non-thermal and thermal loop

  7. Other subjects • Eruptions • Uniform coverage for a long time (weather, good maintenance, one solar cycle), continuum emission, and high cadence • Active regions • Umbral oscillation (solar cycle dependence) • Magnetic field measurements • Quiet sun • Polar brightening, dark filaments/prominences (solar cycle dependence)

  8. Proposal of a new solar flare scenario • NoRH event on 1993 January 2 movie • Two (multiple) loop configuration, non-thermal loop • Ballooning/Flute instability (interchange instability) • Finite(high) beta plasma in a curved magnetic field • Thermal(confined) / flow plasma energy is the energy source for solar flares • Turbulence (power law energy distribution and power law distribution of power spectra of microwave light curves.)

  9. Power law energy distribution N(E)dE = A E-δdE　 log (N) log (E)

  10. A new flare model/scenario Plasma turbulence Plasma/particle Ballooning instability (interchange instability)

  11. International user group • Open data policy • INTERNET development • All the data since the beginning are online • Event lists, event images (Yokoyama) • Ejection lists, images (Shimojo) • NoRH software/SSW and analysis manuals (Yokoyama et al.) • Data analysis opportunities (CDAW like) • Invitation of international users to Nobeyama

  12. Publications • Refereed journals: 120 papers • Proceedings: 194 papers • More publications in refereed journals

  13. Proceedings of this symposium • Electronic files on CD-ROM • Proceedings book (review reports) • Special issue for NoRH: Publication of Astronomical Society of Japan (original contributions+one invited review paper) • We encourage you to submit original papers including NoRH data to PASJ special issue.

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