RT Journal Article
ID 1225db726fefd720
A1 Melnik, V. N.
A1 Konovalenko, Alexandr A.
A1 Rucker, H. O.
A1 Dorovsky, V. V.
A1 Abranin, E. P.
A1 Lecacheux, A.
A1 Lonska, A. S. 
T1 SOLAR S-BURSTS AT DECAMETER WAVELENGTHS
JF Radio Physics and Radio Astronomy
JO RPRA
YR 2010
FD 2010-11-10
VO 1
IS 4
SP 281
OP 289
K1 corona
K1 radio bursts
K1 decameter wavelengths
K1 magnetic field
K1 dynamic spectrum
AB Investigated are properties of S-bursts observed within 10−30 MHz with the UTR-2 radio telescope in 2001−2002. Three storms of these bursts occurred on May 23−26, 2001, July 13−16 and July 27−30, 2002 were selected for a detailed analysis. Altogether, during these storms more than 800 bursts were recorded. The bursts were always observed on the background of enhanced solar activity at decameter wavelengths. Those were the ordinary type III and IIIb bursts, type III-like bursts, drift pairs, and spikes. The S-bursts were observed on the days when the related active region was located near the central meridian. Duration of bursts for every storm remained practically constant, being 0.3 s during the storm of 2001 and 0.4−0.6 s during the storms of 2002. The instantaneous frequency bandwidth of S-bursts has been found increasing with frequency sensibly linearly. The drift rate of S-bursts varies with frequency according to the law close to the one found by McConnell for the bursts at higher frequencies. Offered is the model of generation of S-bursts based on assumption that they are generated due to Langmuir waves coalescence with fast magnetoacoustic waves whose phase and group velocities are equal.
PB Begell House
LK https://www.dl.begellhouse.com/journals/6fd1549c0e2c05da,15826c680ad7d10a,1225db726fefd720.html