The Reflares and Outburst Evolution in the Accreting Millisecond Pulsar SAX J1808.4-3658: a Disk Truncated Near Co-rotation?

TL;DR

This study examines the reflaring states of SAX J1808.4-3658, revealing a stable accretion flow configuration with a truncated disk near the co-rotation radius, influenced by outflows or a trapped disk mechanism.

Contribution

It provides multiwavelength analysis of the reflaring states, suggesting the inner accretion disk is truncated near the co-rotation radius during these phases.

Findings

X-ray luminosity varies by up to three orders of magnitude during reflares.

NIR/optical/UV emission shows shallower luminosity variations compared to X-rays.

The accretion disk is likely truncated at or near the co-rotation radius during reflares.

Abstract

The accreting millisecond X-ray pulsar SAX J1808.4--3658 shows peculiar low luminosity states known as "reflares" after the end of the main outburst. During this phase the X-ray luminosity of the source varies by up to three orders of magnitude in less than 1-2 days. The lowest X-ray luminosity observed reaches a value of ~1e32 erg/s, only a factor of a few brighter than its typical quiescent level. We investigate the 2008 and 2005 reflaring state of SAX J1808.4-3658 to determine whether there is any evidence for a change in the accretion flow with respect to the main outburst. We perform a multiwavelength photometric and spectral study of the 2005 and 2008 reflares with data collected during an observational campaign covering the near-infrared, optical, ultra-violet and X-ray band. We find that the NIR/optical/UV emission, expected to some from the outer accretion disk shows variations in luminosity which are 1--2 orders of magnitude shallower than in X-rays. The X-ray spectral state observed during the reflares does not change substantially with X-ray luminosity indicating a rather stable configuration of the accretion flow. We investigate the most likely configuration of the innermost regions of the accretion flow and we infer an accretion disk truncated at or near the co-rotation radius. We interpret these findings as due to either a strong outflow (due to a propeller effect) or a trapped disk (with limited/no outflow) in the inner regions of the accretion flow.