Superburst Models for Neutron Stars with Hydrogen and Helium-Rich Atmospheres

TL;DR

This study models superbursts on neutron stars with hydrogen and helium atmospheres, revealing complex burning behaviors and shorter quenching times than previously thought, with implications for understanding X-ray burst recurrence.

Contribution

First comprehensive multi-zone models of superbursts including hydrogen and helium burning, analyzing transition regimes and quenching times in neutron star atmospheres.

Findings

Superbursts quench sooner than previously predicted due to complex reaction interplay.

Stable hydrogen and helium burning transitions through marginally stable burning (mHz QPOs).

Identified shortest quenching time for 4U 1636-536 using observational data.

Abstract

Superbursts are rare day-long Type I X-ray bursts due to carbon flashes on accreting neutron stars in low-mass X-ray binaries. They heat the neutron star envelope such that the burning of accreted hydrogen and helium becomes stable, and the common shorter X-ray bursts are quenched. Short bursts reappear only after the envelope cools down. We study multi-zone one-dimensional models of the neutron star envelope, in which we follow carbon burning during the superburst, and we include hydrogen and helium burning in the atmosphere above. We investigate both the case of a solar composition and a helium-rich atmosphere. This allows us to study for the first time a wide variety of thermonuclear burning behavior as well as the transitions between the different regimes in a self-consistent manner. For solar composition, burst quenching ends much sooner than previously expected. This is because of the complex interplay between the 3-alpha, hot CNO, and CNO breakout reactions. Stable burning of hydrogen and helium transitions via marginally stable burning (mHz QPOs) to less energetic bursts with short recurrence times. We find a short-lived bursting mode where weaker and stronger bursts alternate. Eventually the bursting behavior changes back to that of the pre-superburst bursts. Because of the scarcity of observations, this transition has not been directly detected after a superburst. Using the MINBAR burst catalog we identify the shortest upper limit on the quenching time for 4U 1636-536, and derive further constraints on the time scale on which bursts return.