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Simulating the Collapse of a Thick Accretion Disk due to a Type I X-Ray Burst from a Neutron Star

  • Authors: P. Chris Fragile, David R. Ballantyne, Thomas J. Maccarone, and Jason W. L. Witry

2018 The Astrophysical Journal Letters 867 L28.

  • Provider: AAS Journals

Caption: Figure 3.

Spacetime diagram of the ratio between the density-weighted orbital angular frequency for simulations with and without a Type I X-ray burst. The orbital frequencies of the two disks are nearly identical until ≈0.75 s, when the simulation with the burst begins to orbit at less than the Keplerian frequency. The ratio continues to decline all through the disk as the burst luminosity grows. This result indicates that an additional torque is acting on the gas that is growing with the burst luminosity, which is exactly the hallmark of PR drag.

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