AbstractIndividual giant radio pulses (GRPs) from the Crab pulsar last only a few microseconds. However, during that time they rank among the brightest objects in the radio sky reaching peak flux densities of up to 1500Jy even at high radio frequencies. Our observations show that GRPs can be found in all phases of ordinary radio emission including the two high frequency components (HFCs) visible only between 5 and 9GHz [Moffett, D.A., Hankins, T.H. Multifrequency radio observations of the Crab pulsar. Astrophys. J. 468, 779–783, 1996]. This leads us to believe that there is no difference in the emission mechanism of the main pulse (MP), inter pulse (IP) and HFCs. High resolution dynamic spectra from our recent observations of giant pulses with the Effelsberg telescope at a center frequency of 8.35GHz show distinct spectral maxima within our observational bandwidth of 500MHz for individual pulses. Their narrow band components appear to be brighter at higher frequencies (8.6GHz) than at lower ones (8.1GHz). Moreover, there is an evidence for spectral evolution within and between those structures. High frequency features occur earlier than low frequency ones. Strong plasma turbulence might be a feasible mechanism for the creation of the high energy densities of ∼6.7×104ergcm−3 and brightness temperatures of ∼1031K.
Giant radio pulses from the Crab pulsar
Advances in Space Research ; 35 , 6 ; 1166-1171
2005-01-28
6 pages
Article (Journal)
Electronic Resource
English
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