Overview of Solar Eruptive Flares
Yoichiro Hanaoka
Abstract
From the viewpoint of solar physics, the solar eruptive flares are a large
scale restructuring of the coronal magnetic field near the solar surface.
There are two major topic in the study of the magnetic field of solar eruptive
flares; one is the energy build-up which eventually causes eruptive phenomena,
and the other one is the energy release and the magnetic field structure
of on-going eruptive phenomena. During recent several years, the
new observations of eruptive phenomena becomes available particularly with
the sophisticated instruments such as Yohkoh and SOHO. Then, the
magnetic field structure of on-going eruptive phenomena -- flares with
ejections, prominence eruptions, and CMEs -- has been widely discussed,
and great progress was made in understanding reconnection in the eruptive
phenomena. On the other hand, the energy build-up due to the evolution
of photospheric magnetic field is not very clear. However, the combination
of coronal images (taken with Yohkoh/SXT, SOHO/EIT, and TRACE), which show
coronal magnetic structure, and photospheric magnetic field data (taken
with SOHO/MDI) enable us to make an advanced study of the energy build-up
process of the eruptive flares.
In my talk, I would like to discuss mainly on the eruptive solar flares
from the viewpoint of solar physics, particularly on the recent progress
of the energy build-up study of the eruptive events.
Organization: National Astronomical Observatory of Japan
Telephone: +81-422-34-3730
Fax: +81-422-34-3742
e-mail: hanaoka@nro.nao.ac.jp
Address: 2-21-1 Osawa, Mitaka
Tokyo 181-8588
Japan