Evidence of non-Solar elemental composition in the clocked X-ray burster SRGA J144459.2$-$604207

TL;DR

This study presents evidence that the X-ray burster SRGA J144459.2-604207 has a non-solar elemental composition, based on modeling its burst light curves, marking a first in clocked bursters.

Contribution

The paper introduces multizone X-ray burst models with non-solar compositions that successfully reproduce observed behaviors, suggesting this is the first clocked burster with non-solar elemental makeup.

Findings

Higher CNO metallicity models fit the observed burst decline.

A helium-enhanced composition with X/Y ≈ 1.5 is preferred.

Non-solar compositions can explain unique burst features.

Abstract

In February and March 2024, a series of many Type I X-ray bursts from the accreting neutron star SRGA J144459.2$-$604207, which has been identified by multiple X-ray satellites, with the first reports coming from INTEGRAL and NinjaSat. These observations reveal that after exhibiting very regular behavior as a ``clocked'' burster, the peak luminosity of the SRGA J144459.2$-$604207 X-ray bursts shows a gradual decline. The observed light curves exhibit a short plateau feature, potentially with a double peak, followed by a rapid decay in the tail-features unlike those seen in previously observed clocked bursters. In this study, we calculate a series of multizone X-ray burst models with various compositions of accreted matter, specifically varying the mass fractions of hydrogen ($X$), helium ($Y$), and heavier CNO elements or metallicity ($Z_{\rm CNO}$). We demonstrate that a model with higher $Z_{\rm CNO}$ and/or lower $X/Y$ compared to the solar values can reproduce the observed behavior of SRGA J144459.2$-$604207. Therefore, we propose that this new X-ray burster is likely the first clocked burster with non-solar elemental compositions. Moreover, based on the X-ray burst light curve morphology in the decline phase observed by NinjaSat, a He-enhanced model with $X/Y \approx 1.5$ seems preferred over high-metallicity cases. We also give a brief discussion on the implications for the neutron star mass, binary star evolution, inclination angle, and the potential for a high-metallicity scenario, the last of which is closely related to the properties of the hot CNO cycle.