The INTEGRAL/SPI view of A0535+26 during the giant outburst of February 2011

TL;DR

This study analyzes the 2011 giant outburst of A0535+26 using INTEGRAL/SPI data, revealing a positive correlation between cyclotron line energy and flux, pulsar spin-up, and flux-dependent pulse profile changes, providing insights into accretion regimes.

Contribution

It presents the first detailed spectral and timing analysis of A0535+26 during a high flux outburst, highlighting the flux-dependent behavior of cyclotron lines and accretion geometry.

Findings

Cyclotron line energy correlates with flux, confirming sub-critical accretion.

Pulsar spins up during the outburst, with spin-up rate linked to flux.

Pulse profile becomes highly asymmetric at high luminosity.

Abstract

A0535+26 is a slowly rotating pulsar accreting from the wind of a massive Be star, and that exhibits two cyclotron absorption lines in its X-ray spectrum, at about 45 and 100 keV, respectively. Unlike similar sources, no significant variations of the energy of its cyclotron lines with flux were observed to date. The bright outburst of February 2011 thus offers a unique occasion to probe this peculiar behavior at flux levels not yet observed with present-day instruments. Here we report on the spectral and timing analysis of the data from the spectrometer SPI on-board INTEGRAL collected during the outburst. At the peak of the outburst the estimated luminosity is ~4.9x10^37 erg/s. The fundamental cyclotron feature is detected at all flux levels, and its centroid energy is positively-correlated with the flux of the source, confirming that A0535+26 is accreting at a sub-critical regime. The correlation seems to fall off at ~10^37 erg/s, suggesting the transition from a Coulomb-stopping regime to a gas-mediated shock regime. From the timing analysis we found that the pulsar was spinning up during most of the outburst, and that the spin-up rate correlates with the flux of the source, albeit the correlation is steeper than the one expected from the standard disk accretion theory. Finally, we show that the pulse profile of the source changes dramatically as the flux increases. At high luminosity the profile is highly asymmetric, implying an asymmetry in the geometry of the accretion flow.