Abstract
Pulsars are rapidly rotating and highly magnetized neutron stars, that radiate non-thermal radio beams from their magnetic poles. The radio emission of pulsars generally remains stable over ∼1,000 averaging pulses, but some pulsars exhibit interesting features in emission variations on short and long timescales. Here, we report an update on the analysis of the phase-resolved pulse-to-pulse energy distribution of PSR J1825-0935, which has two different emission modes, Bright and Quiet modes. We analyze the energy distribution of each mode separately and found that the pulse profile’s main component energy distribution is well described by a log-normal distribution in the Bright mode and inconclusive for the Quiet mode.
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