Giant pulses in pulsar PSR B0031–07
Pushchino Radio Astronomy Observatory, Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences, Pushchino 142290, Russia e-mail: firstname.lastname@example.org
2 Isaac Newton Institute, Chile, Pushchino Branch, Russia
Accepted: 15 July 2004
We report on observations of the recently detected (Kuzmin et al. [CITE]) giant pulses (GPs) from the pulsar PSR B0031–07 at 40 and 111 MHz. At 40 MHz the peak flux density of the strongest pulse is 1100 Jy, which is 400 times as high as the peak flux density of the average pulse (AP). A pulse whose observed peak flux exceeded the peak of the AP by more than a factor of 200 is encountered approximately once in 800 observed periods. Peak flux density of the GPs compared to the AP peak flux density has roughly a power-law distribution with a slope of -4.5. GPs at 40 MHz are essentially stronger than those ones at 111 MHz. This excess is approximately in inverse proportion to the frequency ratio. The giant pulses are much narrower than the AP, and cluster in two narrow regions of the AP near the peaks of the two components of the AP. Some of the GPs emit at both phases and are double. The separation of the double GP emission regions depends on frequency. Similarly to the frequency dependence of the width of the AP, it is less at 111 MHz than at 40 MHz. This suggests that GPs are emitted from the same region of the magnetosphere as the AP, that is in a hollow cone over the polar cap instead of the light cylinder region. PSR B0031–07 as well as the previously detected PSR B1112+50 are the first pulsars with GPs that do not have a high magnetic field at the light cylinder. One may suggest that there are two classes of GPs, one associated with high-energy emission from outer gaps, the other associated with polar radio emission. The GPs of PSR B0031–07 and PSR B1112+50 are of the second class. The dispersion measure DM is found to be .
Key words: stars: neutron / stars: pulsars: general / stars: pulsars: individual: PSR B0031–07
© ESO, 2004