Pulse-to-Pulse Spectroscopy of Bright Accreting Pulsars

Details Pulse-to-Pulse Spectroscopy of Bright Accreting Pulsars Pulse-to-Pulse Spectroscopy of Bright Accreting Pulsars

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011head...12.4204k&link_type=abstract

American Astronomical Society, HEAD meeting #12, #42.04

Physics

Scientific paper

In our work we concentrate on the variability of single X-ray pulses (i.e., their changes from one pulsation cycle to the next) exhibited by many accreting pulsars and often referred to as pulse-to-pulse variability. Such a variability is believed to be due to a highly non-stationary accretion flow close to the neutron star surface leading to short-time-scale variations in the mass accretion rate. The high-quality data taken with RXTE and INTEGRAL on a sample of bright transient and persistent pulsars allow us for the first time to reveal and study variability of the broad-band X-ray spectrum as a function of amplitude of single X-ray pulses (combining all the pulses in a particular amplitude bin). Our approach, which we call "pulse-to-pulse spectroscopy", allowed us to probe the physics inside the X-ray emitting structure (accretion column/mound) by studying its reaction on the short-term variations of the mass accretion rate. As a result, we found two types of spectral behavior of the sources which we interprete as a manifestation of two distinct accretion regimes. The regime realized in a particular pulsar depends on whether its averaged X-ray luminosity is above or below some critical value which depends on the pulsar parameters.

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