# Evidence for the radiation-pressure dominated accretion disk in bursting pulsar GRO J1744-28 using timing analysis

## TL;DR

This study analyzes timing data from the X-ray pulsar GRO J1744-28 to provide evidence that its accretion disk is dominated by radiation pressure during super-Eddington outbursts, challenging canonical models.

## Contribution

It presents observational evidence and a qualitative model indicating the presence of a radiation-pressure dominated accretion disk in GRO J1744-28 at high luminosities.

## Key findings

- Observed PDS break frequency exceeds expectations from magnetic field estimates.
- The PDS shape differs from canonical models, indicating different disk dynamics.
- Weak luminosity dependence of the inner disk radius supports radiation-pressure dominance.

## Abstract

The X-ray pulsar GRO J1744-28 is a unique source which shows both pulsations and type-II X-ray bursts, allowing studies of the interaction of the accretion disk with the magnetosphere at huge mass accretion rates exceeding $10^{19}$ g s$^{-1}$ during its super-Eddington outbursts. The magnetic field strength in the source, $B\approx 5\times 10^{11}$ G, is known from the cyclotron absorption feature discovered in the energy spectrum around 4.5 keV. Here, we explore the flux variability of the source in context of interaction of its magnetosphere with the radiation-pressure dominated accretion disk. Particularly, we present the results of the analysis of noise power density spectra (PDS) using the observations of the source in 1996-1997 by RXTE. Accreting compact objects commonly exhibit a broken power-law shape of the PDS with a break corresponding to the Keplerian orbital frequency of matter at the innermost disk radius. The observed frequency of the break can thus be used to estimate the size of the magnetosphere. We found, however, that the observed PDS of GRO J1744-28 differs dramatically from the canonical shape. Furthermore, the observed break frequency appears to be significantly higher than what is expected based on the magnetic field estimated from the cyclotron line energy. We argue that these observational facts can be attributed to the existence of the radiation-pressure dominated region in the accretion disk at luminosities above $\sim$2$\times 10^{37}$ erg s$^{-1}$. We discuss a qualitative model for the PDS formation in such disks, and show that its predictions are consistent with our observational findings. The presence of the radiation-pressure dominated region can also explain the observed weak luminosity-dependence of the inner radius, and we argue that the small inner radius can be explained by a quadrupole component dominating the magnetic field of the neutron star.