Interstellar scattering causes broadening and distortion in the mean pulse profiles and polarization position angle(PPA)curves of pulsars,especially pulse profiles observed at lower frequencies.This paper implements a method to recover the pulse profiles and PPA curves of five pulsars which have obvious scattered pulse profiles at lower frequency.It reports a simulation to show the scattering and descattering of pulse profiles and PPA curves,and as a practical application the lower frequency profiles and PPA curves of PSR 1356-60,PSR 1831-03,PSR 1838+04,PSR 1859+03 and PSR 1946+35 are obtained.It is found that the original pulse profiles and PPA curves can be recovered.
We present an analysis of strong single pulses from PSR J0034-0721. Our observations were made using the Urumqi 25-m radio telescope at a radio frequency of 1.54GHz. A total of 353 strong pulses were detected during eight hours of observing. The signal-to-noise ratios of the detected pulses range from 5 to 11.5. The peak fluxes of those pulses are 17 to 39 times that of the average pulse peak. The cumulative distribution of the signal-to-noise ratios of these strong pulses has a rough power-law distribution with a slope of 4.4 ± 0.5. Ten of the strong pulses arrived approximately 23 to 40 ms earlier than the average profile peak. This suggests the possibility that there are two strong pulse-emitting regions.
We report on the properties of strong pulses from PSR B0656+14 by analyzing the data obtained using the Urumqi 25-m radio telescope at 1540 MHz from August 2007 to September 2010.In 44 h of observational data,a total of 67 pulses with signal-to-noise ratios above a 5σthreshold were detected.The peak flux densities of these pulses are 58 to 194 times that of the average profile,and their pulse energies are 3 to 68 times that of the average pulse.These pulses are clustered around phases about 5-ahead of the peak of the average profile.Compared with the width of the average profile,they are relatively narrow,with the full widths at half-maximum ranging from 0.28 ° to 1.78 °.The distribution of pulse-energies follows a lognormal distribution.These sporadic strong pulses detected from PSR B0656+14 have different characteristics from both typical giant pulses and its regular pulses.
Guo-Cun TaoAli EsamdinHui-Dong HuMao-Fei QianJing LiNa Wang
