X-ray outbursts of low-mass X-ray binary transients observed in the RXTE era

TL;DR

This study analyzes 110 bright X-ray outbursts from 36 low-mass X-ray binary transients observed with RXTE, revealing correlations between outburst properties and differences between black hole and neutron star systems, suggesting common underlying mechanisms.

Contribution

It provides a comprehensive statistical analysis of outburst properties, identifying key correlations and differences that help distinguish the nature of compact objects and understand outburst mechanisms.

Findings

Black hole LMXBTs have at least twice the average peak luminosity of neutron star LMXBTs.

Outburst peak luminosity correlates with the rate of change of luminosity during rise and decay.

Similar outburst mechanisms may operate in ULXs in M31, reaching Eddington luminosity.

Abstract

We have performed a statistical study of the properties of 110 bright X-ray outbursts in 36 low-mass X-ray binary transients (LMXBTs) seen with the All-Sky Monitor (2--12 keV) on board the {\it Rossi X-ray Timing Explorer} ({\it RXTE}) in 1996--2011. We have measured a number of outburst properties, including peak X-ray luminosity, rate of change of luminosity on a daily timescale, $e$-folding rise and decay timescales, outburst duration, and total radiated energy. We found that the average properties such as peak X-ray luminosity, rise and decay timescales, outburst duration, and total radiated energy of black hole LMXBTs, are at least two times larger than those of neutron star LMXBTs, implying that the measurements of these properties may provide preliminary clues as to the nature of the compact object of a newly discovered LMXBT. We also found that the outburst peak X-ray luminosity is correlated with the rate of change of X-ray luminosity in both the rise and the decay phases, which is consistent with our previous studies. Positive correlations between total radiated energy and peak X-ray luminosity, and between total radiated energy and the $e$-folding rise or decay timescale, are also found in the outbursts. These correlations suggest that the mass stored in the disk before an outburst is the primary initial condition that sets up the outburst properties seen later. We also found that the outbursts of two transient stellar-mass ULXs in M31 also roughly follow the correlations, which indicate that the same outburst mechanism works for the brighter outbursts of these two sources in M31 that reached the Eddington luminosity.