The observational evidence of solar coronal decimetric radio pulsations with very short periods

Details The observational evidence of solar coronal decimetric radio pulsations with very short periods The observational evidence of solar coronal decimetric radio pulsations with very short periods

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003acasn..44..139x&link_type=abstract

Acta Astronomica Sinica, vol. 44, no. 2, p. 139-146

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1

Sun: Coronal, Sun: Magnetic Fields, Sun: Radio Radiation

Scientific paper

Two rare events were observed with the decimetric (700---1500MHz) radio spectrometer and the synchronous observational system with high temporal resolution at four frequencies (1420, 2130, 2840, and 4260MHz) at Yunnan Observatory, National Astronomical Observatories of China on June 24, 2001 and July 30, 1990, respectively. The former is a small radio burst, associated with the pulsations with short periods (about 30, 40, and 100 milliseconds) in impulsive phase. The latter is a great radio burst, with the periods of the order of 30 milliseconds at 2840MHz. In this paper, the pulsations with very short periods of the order of 29---40 milliseconds are mainly emphasized and discussed. Such radio emission pulsations with very short periods may be generated by the modulation of the periodic trains of whistler packets originating in unstable region in the corona. Alternatively, these pulsations may be attributed to the wave-wave nonlinear interactions when a beam of precipitating electrons in a flaring loop drives electrostatic upper hybrid waves. These electrostatic waves can interact coherently with each other via the nonlinear oscillations to produce electromagnetic radiation with the periods of about 30 milliseconds at twice upper hybrid frequency.

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