Search for the Giant Pulses - an extreme phenomenon in radio pulsar emission

Slow pulse-to-pulse variation of intensity is very typical for overwhelming majority of known pulsars. However, a handful of pulsars have mysterious mechanism which can break such a stability. Phenomenon of generation GPs was first detected for Crab pulsar(B0531+21) [1] and the millisecond pulsar B1937+21 [2]. In following studies a set of typical characteristics of GPs was determined. These are: very narrow components in pulse’s microstructure (up to several nanoseconds), high peak flux density(up to several MJy), and power-law distribution of the peak flux density of GPs. It is important to emphasize, that the pulsar B0531+21 and B1937+21 have very strong magnetic field on the light cylinder (BLC ≈ 106 G) and are considered as ”classical” pulsars with GPs. In course of time, GPs were detected from 5 pulsars with very strong magnetic field on the light cylinder (BLC ≈ 105 − 106 G): B0218+42 [3], B0540-69 [4], B1821-24 [5], J1823-3021 [6] and B1957+20 [3]. However, later on similar phenomenon was detected (mostly at low radio frequencies between 40 and 111 MHz) for set of pulsars with a value of BLC from several to several hundreds gauss: J0034-0721 [7], J0529-6652 [8], J0659+1414 [9], J0953+0755 [10, 11], J1115+5030 [12] and J1752+2359 [13]. In present work we describe the results of our observations that were held to search for new pulsars generating GPs or anomalous strong pulses at low radio frequencies.