Weak Bursts on Slowly Accreting Neutron Stars

TL;DR

This paper investigates the conditions under which weak hydrogen bursts occur on slowly accreting neutron stars, revealing that high metallicity can trigger convection and produce observable burst features similar to those seen in SAX J1808.4-3658.

Contribution

It demonstrates through stellar modeling that elevated metallicity in accreted material can cause unstable hydrogen ignition and convection, explaining observed weak bursts.

Findings

High metallicity leads to convection and sharp luminosity peaks.

Extended tail of emission correlates with hydrogen exhaustion.

Luminosity ratios indicate metallicity gradients in accreted matter.

Abstract

Nearly all observed thermonuclear X-ray bursts are thought to be triggered by the thermally unstable triple-alpha process. Unlike in accreting white dwarfs, the $\gtrsim10^{8} \mathrm{K}$ envelope temperature forces hydrogen burning to proceed via the $\beta$-limited, thermally stable hot CNO cycle. Recent observations of weak X-ray bursts from SAX J1808.4-3658 occurring within 1-3 days of the onset of an accretion outburst have raised the question that these bursts were triggered by thermally unstable hydrogen ignition, analogously to classical novae. Using the stellar evolution code MESA, we explore the unstable ignition of hydrogen on slowly accreting neutron stars. For solar metallicities, the burning is insufficiently vigorous to launch convection and the burst rise is on the envelope thermal timescale, with the hydrogen being consumed over hours. For elevated metallicities ($Z\gtrsim0.06$), however, the initial proton captures onto CNO nuclei heat the envelope enough to drive convection and produce a sharp peak in the luminosity. This peak can match that of the SAX J1808.4-3658 burst, for sufficient enrichment. Following this peak, the hydrogen burning stabilizes at a rate set solely by the ignition depth and CNO abundance in the accreted matter. This quasi-steady-state burning produces an extended tail of elevated emission that lasts until the hydrogen is exhausted. Observations of the tail's luminosity and duration measure the hydrogen and metallicity abundance of the accreted material, while the distance-independent ratio of peak-to-tail luminosities would suggest the presence of significant metallicity gradients prior to convection.