Giant Pulses in Crab and B1133+16

Abstract

Giant Pulses (GP) from pulsars are usually considered to be 10 or more times stronger than the average pulse emitted by the pulsar. The emission mechanism of these pulses are not fully understood yet. The only common aspect of pulsars with GP emission is that they have a high magnetic field at the velocity of light cylinder. So far, GP studies mostly concentrated on the giant pulses from high magnetic field pulsar and pulses with very high signal to noise ratio. With the possibility of high time resolution and flexibilty offered by the Pulsar Machine II (PuMa‐II), an analysis of weak giant pulses, and giant pulses at low frequency from normal pulsars can be undertaken. The default coherent dedispersion used in data reduction is a clear advantage in the study of single pulses at low sky frequencies. We detect giant pulse emission from the nearby low magnetic field pulsar, B1133+16 at low oberving frequencies. Detection of weak giants in the Crab pulsar are greatly aided by the Westerbork Synthesis Radio Telescope(WSRT) and PuMa‐II combination: 1. The synthesized beam of WSRT resolves out the Crab nebula, and reduces the nebular noise contribution. 2. PuMa‐II can record 160 MHz of bandwidth and can coherently dedisperse the full bandwidth giving us an excellent time resolution and sensitivity. We will present results of a study of GPs from the Crab pulsar and PSR B1133+16.