Orbital Period and Outburst Luminosity of Transient Low Mass X-ray Binaries

TL;DR

This study examines how the maximum luminosity during X-ray outbursts in transient low mass X-ray binaries correlates with orbital period, revealing a general increase with period and differences between neutron star and black hole systems at shorter periods.

Contribution

It provides empirical evidence linking outburst luminosity to orbital period and compares neutron star and black hole systems, aligning observations with theoretical models.

Findings

Luminosity generally increases with orbital period.

No significant luminosity difference between neutron star and black hole systems above 4h.

Potential higher peak luminosities in ultra-compact binaries.

Abstract

In this paper we investigate the relation between the maximal luminosity of X-ray outburst and the orbital period in transient low mass X-ray binaries (or soft X-ray transients) observed by the Rossi X-ray Timing Explorer (RXTE) in the past decade. We find that the maximal luminosity (3-200 keV) in Eddington unit generally increases with increasing orbital period, which does not show a luminosity saturation but in general agrees with theoretical prediction. The peak luminosities in ultra-compact binaries might be higher than those with orbital period of 2-4 h, but more data are needed to make the claim. We also find that there is no significant difference in the 3-200 keV outburst peak luminosity between neutron star systems and black hole systems with orbital periods above 4 h; however, there might be significant difference at smaller orbital period where only neutron star systems are observed and radiatively ineffcient accretion flow is expected to work at the low luminosities for black hole accreters.