Volume 383, Number 3, MarchI 2002
|Page(s)||1018 - 1031|
|Section||Planets and planetary systems|
|Published online||15 March 2002|
X-ray observations of a large-scale solar coronal shock wave
Mullard Space Science Laboratory, University College London, Holmbury Saint Mary, Dorking, Surrey, RH5 6NT, UK
2 Institute of Space & Astronautical Science, 3–1–1 Yoshinodai, Sagamihara, Kanagawa 229–8510, Japan
3 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
Corresponding author: J. I. Khan, email@example.com
Accepted: 27 November 2001
We report observations of a propagating disturbance in the solar corona observed in emission in soft X-ray images from the Yohkoh Soft X-ray Telescope (SXT). The disturbance was associated with a flare which began at about 09:04 UT on 1997 November 03. This flare was associated with a type II radio burst observed at decimetric-dekametric wavelengths by the Astrophysikalisches Institut Potsdam Radio Spectrograph. Hα data from Kanzelhöhe Solar Observatory show that a Moreton wave was associated with this event. Moreover, Solar and Heliospheric Observatory Extreme Ultraviolet Imaging Telescope (EIT) 195 Å data show an `EIT wave' associated with this event. Extrapolations of the leading edge of the propagating soft X-ray disturbance show a close association with both of these wave features. The soft X-ray disturbance is observed to travel with a speed of about 546 km s-1. Using Nançay Radioheliograph data we directly determine the source locations of the type II radio burst. These are found to be located close to the soft X-ray disturbance and show motions consistent with the soft X-ray motions. These results lead us to conclude that the “SXT wave” is the coronal counterpart of a Moreton wave, analogous to EIT waves, i.e., it is the first confirmed direct observation of a solar coronal shock wave in X-rays.
Key words: Sun: corona / Sun: flares / Sun: radio radiation / Sun: UV radiation / Sun: X-rays, gamma rays / shock waves
© ESO, 2002
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