Application of the relativistic precession model to the accreting millisecond X-ray pulsar IGR J17511-3057

TL;DR

This paper applies the relativistic precession model to twin kHz QPOs observed in the accreting millisecond X-ray pulsar IGR J17511-3057, revealing inconsistencies among different observation groups and a broad QPO formation region.

Contribution

It demonstrates the application of the relativistic precession model to multiple observation groups of a specific pulsar, highlighting discrepancies and the extent of the QPO formation region.

Findings

Predictions from one observation group conflict with others.

The QPO formation region is broad and extends beyond the ISCO.

Discrepancies challenge the model's universality.

Abstract

The observation of a pair of simultaneous twin kHz QPOs in the power density spectrum of a neutron star or a black hole allows its mass-angular-momentum relation to be constrained. Situations in which the observed simultaneous pairs are more than one allow the different models of the kHz QPOs to be falsified. Discrepancy between the estimates coming from the different pairs would call the used model into question. In the current paper the relativistic precession model is applied to the twin kHz QPOs that appear in the light curves of three groups of observations of the accreting millisecond X-ray pulsar IGR J17511-3057. It was found that the predictions of one of the groups are practically in conflict with the other two. Another interesting result is that the region in which the kHz QPOs have been born is rather broad and extends quite far from the ISCO.