Astron. Astrophys. 343, 287-296 (1999)

Radio evidence on shock wave formation in the solar corona

A. Klassen ¹, H. Aurass ¹, K.-L. Klein ², A. Hofmann ¹ and G. Mann <sup>1

1</sup> Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany
² Observatoire de Paris, Section de Meudon, DASOP and URA 2080, F-92195 Meudon Principal Cedex, France

Received 27 August 1998 / Accepted 2 December 1998

Abstract

In order to investigate the formation of radio emitting shock waves above flaring active regions, we combine spectral and imaging observations of type II radio events with X-ray imaging and full-Sun observations and, in one case, with the extrapolated magnetic field configuration in the corona. We confirm and extend earlier findings that type II bursts are emitted above active region loops seen in soft X-ray images. Sources at successively lower frequencies are non-radially displaced from the axis of the active region loops. Two new radio features identified in high resolution spectrograms establish a possible link between the type II emission and the preceding activity in the underlying corona:

1. Groups of fast drift bursts or pulsations with a restricted bandwidth are observed in coronal loops from the impulsive flare phase until the onset of the type II emission. These groups or their high frequency cut-off are found in the spectral range around the backward extrapolated type II lanes. Envelope features of the group (starting frequency and/or cut-off frequency) drift gradually to lower frequencies, at a normalized drift rate similar to the following type II lanes. The sources are located between the sites of H emission and of the type II emission. We refer to this burst group and its envelope features as a type II precursor .

2. Immediately before the type II emission a short ( 1 min duration) series of narrow-band bursts occurs at frequencies between the split bands of the type II lanes. As a whole, the burst sequence has an inverted U-shaped spectral envelope. We therefore call it an arc . It has fundamental-harmonic structure as the subsequent type II burst, but no band split. The source is located near or above the summits of the coronal loops where the precursor emission occurred before, and close to the site where the type II emission starts. The arc feature occurs especially prior to high frequency type II bursts, i.e. type II shocks formed at comparatively low coronal height.

It is concluded that the type II burst is related to a plasma jet or a blast wave that originates in closed magnetic structures in the active region, and is first recognized during the early impulsive phase (between the onset and main maximum of the hard X-ray emission). This disturbance becomes or launches a shock wave when it attains the summit of these structures. The shock is refracted into overlying field regions, where it becomes visible through the type II emission.

Key words: shock waves Sun: corona Sun: flares Sun: magnetic fields Sun: radio radiation

Send offprint requests to: A. Klassen (aklassen@aip.de)

This article contains no SIMBAD objects.

Contents

• 1. Introduction
• 2. The observations
  • 2.1. Instruments and data selection
  • 2.2. Description of individual events
    • 2.2.1. 13 July 1994
    • 2.2.2. 27 September 1993
    • 2.2.3. 27 December 1993
    • 2.2.4. 28 December 1993
    • 2.2.5. 7 July 1994
  • 2.3. Summary of observational results
• 3. Discussion
  • 3.1. Type II source location
  • 3.2. Type II precursor features
  • 3.3. The arc
• Acknowledgements
• References

© European Southern Observatory (ESO) 1999

Online publication: March 1, 1999
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