# An enigmatic hump around 30 keV in Suzaku spectra of Aquila X-1 in the Hard State

## TL;DR

This study reports a mysterious 30 keV hump in Suzaku spectra of Aquila X-1 in the hard state, suggesting atomic features from heavy elements synthesized during thermonuclear flashes.

## Contribution

It identifies and models a unique spectral excess around 30 keV in neutron star spectra, proposing explanations involving Gaussian and recombination edge models.

## Key findings

- The 30 keV feature is statistically significant.
- The feature can be modeled as a Gaussian or a recombination edge.
- The results relate to heavy element atomic features from thermonuclear processes.

## Abstract

The typical accreting neutron star, Aquila X-1, was observed with Suzaku seven times in the decay phase of an outburst in 2007 September-October. Among them, the second to the fourth observations were performed 10 to 22 days after the outburst peak, when the source was in the hard state with a luminosity of 2x10^36 erg/sec. A unified spectral model for this type of objects approximately reproduced the 0.8--100~keV spectra obtained in these 3 observations. However, the spectra all exhibited an enigmatic hump-like excess around 30 keV, above the hard X-ray continuum which is interpreted as arising via Comptonization. The excess feature was confirmed to be significant against statistical and systematic uncertainties. It was successfully represented by a Gaussian centered at ~32 keV, with a width (sigma) of ~6 keV and an equivalent width of ~8.6 keV. Alternatively, the feature can also be explained by a recombination edge model, that produces a quasi-continuum above an edge energy of ~27 keV with an electron temperature of ~11 keV and an equivalent width of ~6.3 keV. These results are discussed in the context of atomic features of heavy elements synthesized via rapid-proton capture process during thermonuclear flashes.