# The Radiation Structure of PSR B2016$+$28 Observed with FAST

## TL;DR

This study uses FAST to analyze PSR B2016+28's pulse structures, revealing frequency-dependent mean pulses, stable single-pulse structures, and correlations in drifting sub-pulses, providing insights into pulsar magnetosphere dynamics.

## Contribution

First detailed analysis of PSR B2016+28 with FAST, demonstrating frequency-dependent pulse profiles and evidence supporting the RS-type vacuum inner gap model.

## Key findings

- Mean pulse profiles fit a conal model
- Pulse width decreases with frequency by ~20%
- Correlation between modulation period and sub-pulse separation

## Abstract

With the largest dish Five-hundred-meter Aperture Spherical radio Telescope (FAST), both the mean and single pulses of PSR B2016$+$28, especially including the single-pulse structure, are investigated in detail in this study. The mean pulse profiles at different frequencies can be well fitted in a conal model, and the peak separation of intensity-dependent pulse profiles increases with intensity. The integrated pulses are obviously frequency dependent (pulse width decreases by $\sim\,20\%$ as frequency increases from 300 MHz to 750 MHz), but the structure of single pulses changes slightly (the corresponding correlation scale decreases by only $\sim\,1\%$). This disparity between mean and single pulses provides independent evidence for the existence of the RS-type vacuum inner gap, indicating a strong bond between particles on the pulsar surface. Diffused drifting sub-pulses are analyzed. The results show that the modulation period along pulse series ($P_3$) is positively correlated to the separation between two adjacent sub-pulses ($P_2$). This correlation may hint a rough surface on the pulsar, eventually resulting in the irregular drift of sparks. All the observational results may have significant implications in the dynamics of pulsar magnetosphere and are discussed extensively in this paper.