Volume 380, Number 1, December II 2001
|Page(s)||318 - 322|
|Section||Planets and planetary systems|
|Published online||15 December 2001|
Centimetric type N and type M bursts
Yunnan Observatory, National Astronomical Observatories, Chinese Academy of Science, Kunming 650011, PR China
2 National Astronomical Observatories, Chinese Academy of Science, Beijing 100012, PR China e-mail: firstname.lastname@example.org
Corresponding author: M. Wang, email@example.com
Accepted: 27 June 2001
Two special fine structures observed with the 5.2-7.6 GHz high temporal and spectral resolution spectrometer of Beijing Astronomical Observatory (BAO) are described and analyzed in this paper. Because they appear as the letters N and M on dynamic spectra, we call them centimetric type N and type M bursts, respectively. They have very short durations (about 500 ms and 300 ms), small flux densities (tens of SFU), narrow bandwidth (relative bandwidth about 10% ), and very small polarization degree (close to the accuracy limit of observation instruments), but each branch has considerable high frequency drift rates (several GHz/s). We think that they are an extension of metric or decimetric type U(N) bursts in centimetric wavelengths. Type N and type M bursts may be due to the mirroring effect near the foot point, as well as a scattering effect caused by whistler wave turbulence near the top of loop. They may also be interpreted by the quasi-periodic particle injection into coronal loops.
Key words: Sun: activity / Sun: corona / Sun: general / Sun: radio radiation
© ESO, 2001
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