| 著者名 | Authors | 所属機関名 | 所属機関名(欧文) | |
| 1 | #横辺/篤史 | Yokobe/Atsushi | K1 | Solar-Terrestrial Environment Laboratory, Nagoya University |
| 2 | F2 | Kojima/M. | K2 | Solar-Terrestrial Environment Laboratory, Nagoya University |
| 3 | F3 | Ohmi/T. | K3 | Solar-Terrestrial Environment Laboratory, Nagoya University |
| 4 | F4 | Tokumaru/M. | K4 | Solar-Terrestrial Environment Laboratory, Nagoya University |
| 5 | F5 | Hakamada/K. | K5 | Department of Engineering Physics, Chubu University |
講演予稿:
Whole Sun Month(1996年8月10日〜9月8日)期間中の惑星間空間
シンチレーション(IPS)による太陽風速度データとコロナグラフ
観測データの比較解析を行った。この際、IPS、コロナグラフの
いずれの観測データも視線積分の効果を受けているため、計算機
トモグラフィー法を応用して解析を行い、バイアスを除去した。
本講演では、太陽風流源領域における密度の太陽風加速に対する
寄与や同じく太陽風流源領域において太陽風の速度構造が形成さ
れる過程等について議論する。
abstract:
Interplanetary scintillation (IPS) observations have an
advantage that the solar wind can be observed over a large
three-dimensional volume of space. Recently, a more precise
analysis of solar wind speed data observed by IPS become
available by the application of a computer assisted
tomography (CAT) method. Here, we present the result of
comparison analysis between solar wind speed data obtained
by IPS and coronal densities from SOHO/LASCO and Mark-III
K-coronameter of the MLSO.
This study has been made by using the data taken during
the ``Whole Sun Month'' period (August 10. - September 8.,
1996). We expect that during this period the large scale
coronal features were rather stable since this time was
in the solar activity minimum phase. This fact is
favorable for our study. Coronagraph observation data are
also biased by the effect of line-of-sight integration.
But, the solar corona can be observed under various
directions at different times due to the rotation of the
Sun. Using CAT techniques, the underlying three-dimensional
structure can be reconstructed with an assumption of the
temporal stability and the rigid rotation of the solar
corona.
For this analysis, we have prepared a synoptic map of the
solar wind speed at the source surface (at 2.5 solar radii)
derived from CAT analysis of IPS observation from STELab.
Synoptic maps of coronal densities obtained by applying CAT
to coronagraph observations have also made at several
heights between photosphere and source surface. Solar wind
speeds are traced from the source surface to the height of
the coronagraph observations along the magnetic field lines,
which is determined from the source surface potential field
model. From this comparison, we study how the mass density
in the source region of the solar wind affects the solar
wind acceleration. In addition, we investigate how the
structure of the solar wind is generated at the coronal
base.
キーワード:
太陽風,太陽コロナ密度,コロナ磁場,計算機トモグラフィー法
Keywords:
Solar wind,Coronal Density,Coronal magnetic field,Tomography analysis