Xiao 潇 Zhang 张's research works

Figure 1.  E vs. luminosities of pulsars. Panels (a)-(e) reveal correlation in X-ray band, SX band (<2 keV), HX band (>2 keV), gamma-ray band and radio band, respectively. MSPs and NPs are plotted by violet dots and orange squares, respectively. Blue, violet, and orange lines are best fit of all, millisecond and NPs, respectively. The inverted triangles are upper limits of luminosity. The correlation trend is revealed by Pearson correlation coefficient (r) and Spearman tests (r s and p s ), listed in Table 2. Gray dotted lines represent different values of  / L E X . The orchid dashed line and black dashed-dotted line are fitting results of W. Becker & J. Truemper (1997) and H.-K. Chang et al. (2023), respectively.

Figure 2. X-ray luminosity vs. timing parameters. Panels (a)-(c) reveal a correlation between L X with P,  P and B surf . Panel (d) is a correlation between X-ray luminosity and τ. The gray regions are theoretical lines for = B log 6, 7, 8, ...,14 surf

Figure 3. X-ray luminosity vs. B lc and τ. Dots and legends are the same as Figure 1. Panel (a) is correlation between X-ray luminosity and B lc . Panel (b) is correlation with best fit of B lc and τ in two dimensions.

Figure 4.  -P P diagrams. The values of  P are derived by the relationship that  µ L E X

Possible X-ray Counterparts of GPPS Pulsars

A New X-Ray Census of Rotation Powered Pulsars

March 2025

4 Reads

The Astrophysical Journal

[...]

To date, over 4000 pulsars have been detected. In this study, we identify 231 X-ray counterparts of Australia Telescope National Facility (ATNF) pulsars by performing a spatial cross match across the Chandra, XMM-Newton observational catalogs. This data set represents the largest sample of X-ray counterparts ever compiled, including 98 normal pulsars (NPs) and 133 millisecond pulsars (MSPs). Based on this significantly expanded sample, we re-establish the correlation between X-ray luminosity and spin-down power, given by L X ∝ E ̇ 0.85 ± 0.05 across the whole X-ray band. The strong correlation is also observed in hard X-ray band, while in soft X-ray band there is no significant correlation. Furthermore, L X shows a strong correlation with spin period and characteristic age for NPs. For the first time, we observe a strongly positive correlation between L X and the light cylinder magnetic field ( B lc ) for MSPs, with both NPs and MSPs following the relationship L X ∝ B lc 1.14 , consistent with the outer-gap model of pulsars that explains the mechanism of X-ray emission. Additionally, we investigate potential X-ray counterparts for Galactic Plane Pulsar Snapshot pulsars, finding a lower likelihood of detection compared to ATNF pulsars.

Download

Xiao 潇 Zhang 张’s scientific contributions

What is this page?

Publications (1)