New Explanations for Some Observation Phenomena of the Peak Frequency of Solar Radio Bursts

Details New Explanations for Some Observation Phenomena of the Peak Frequency of Solar Radio Bursts New Explanations for Some Observation Phenomena of the Peak Frequency of Solar Radio Bursts

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...708..445z&link_type=abstract

The Astrophysical Journal, Volume 708, Issue 1, pp. 445-449 (2010).

Astronomy and Astrophysics

Astronomy

1

Sun: Flares, Sun: Radio Radiation

Scientific paper

We present new explanations for some observation phenomena of the peak frequency of solar radio burst spectrum, based on spectrum calculations of gyrosynchrotron radiation in a model of magnetic dipole field. These observation phenomena are: (1) a remarkable constant peak frequency of microwave burst spectrum during their lifetime, (2) a composite CD-type burst with two distinct spectral components respectively peaking in centimeter (cm) and decimeter (dm) ranges, and (3) emission of solar flares in the submillimeter band above 100 GHz (THz) and a new increasing submillimeter spectral component. Our calculation results show that the peak frequency can maintain constant when the energy spectral index δ varies only in the range larger than 3, whereas other parameters hold constant. Two distinct spectral components of the dm and cm ranges of the CD-type burst can be produced simultaneously by the energetic electrons with softer energy spectral index (gsim6) and lower low-energy cutoff (lsim30 keV). The THz burst can be generated by energetic electrons with hard spectral index (~3) and high low-energy cutoff (~250 keV) in intense local magnetic fields (mean value \bar{B} = 2100 G) via gyrosynchrotron emission; while a harder spectral index, a higher low-energy cutoff, and higher magnetic field strength are required for the increasing submillimeter spectral component.

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