On the Correlation Between X-ray Luminosity and Spin-Down Energy Loss in Pulsars

Details On the Correlation Between X-ray Luminosity and Spin-Down Energy Loss in Pulsars On the Correlation Between X-ray Luminosity and Spin-Down Energy Loss in Pulsars

Sep 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001cnoc.conf....5c&link_type=abstract

The Second National Conference on Astrophysics of Compact Objects, held in Bologna (Italy), September 19 - 21, 2001, p. 5

Astronomy and Astrophysics

Astrophysics

Scientific paper

The empirical relation between the X-ray luminosity LX and the rotational energy loss LROT of a sample of 38 radio-pulsar is re- examined in light of the more recent data from ASCA, RXTE, BeppoSAX, Chandra, and XMM. The analysis is an improvment, relative to previous studies, as it includes the statistical errors on the photon number counts and spectral modelling, together with the systematical errors related to uncertainties in the source distance. It is found that a linear scaling of the type log LX = log L0 + log LROT, as early suggested by Beker and Trumper exploring a limited sample of X- ray emitting pulsars at soft energies ( 0.1 and 2.4 keV ) is inadeguate to interpret the data in a statistical satisfactory way. The X-ray luminosities all appear to lie under a line satisfying the scaling relation log LX < 1.5 log LROT. This relation is reproduced even when an explicit dependence on the period and period derivative is included in a two-dimensional statistical analysis. The data show a considerable dispersion of LX. This dispersion is strongly suggestive that other physical parameters not corralted with the period and period derivative need to be included in the theory to account for the observed emission at X-ray energies.

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