Radiation Driven Warping of Accretion Discs Due to X-ray Bursts

TL;DR

This paper investigates how X-ray bursts can induce warping instabilities in accretion discs around neutron stars, potentially explaining observed fluctuations and spectral features during such events.

Contribution

It demonstrates that burst luminosity, duration, and disc viscosity influence warp development, providing a new understanding of disc behavior during X-ray bursts.

Findings

Warps are more likely during intermediate and superbursts with photospheric radius expansion.

Larger disc viscosity increases the likelihood of warp growth.

Warp development can explain observed fluctuations and spectral features during bursts.

Abstract

The outpouring of radiation during an X-ray burst can affect the properties of accretion discs around neutron stars: the corona can cool and collapse, the inner regions can be bled away due to enhanced accretion, and the additional heating will lead to changes in the disc height. In this paper, we investigate whether radiation from bursts can cause the disc to distort through a warping instability. Working in the limit of isotropic viscosity and linear growth, we find that bursts are more likely to drive disc warps when they have larger luminosities and longer durations. Therefore, warps will be most probable during intermediate duration bursts (IMDBs) and superbursts with evidence for photospheric radius expansion. Further, the development of warps depends on the disc viscosity with larger values of $\alpha$ increasing the likelihood of warp growth. We perform time-dependent evolution calculations of the development of warps during Type I bursts and IMDBs. Depending on the initial warp prior to the burst, we find the burst produces warps at $r$ <~ 50 $r_g$ that rapidly grow and decay on second-long timescales, or ones that grow more slowly and cover a large fraction of the disc. The pulsations of warp at small radii appear to have the properties needed to explain the achromatic fluctuations that have been observed during the tails of some IMDBs. The large scale, slowly growing warps could account for the large reflection strengths and absorbing column densities inferred late in the 4U 1820-30 and 4U 1636-53 superbursts.