Simulating extreme-mass-ratio systems in full general relativity

William E. East, Frans Pretorius

Research output: Contribution to journalArticlepeer-review

13 Scopus citations

Abstract

We introduce a new method for numerically evolving the full Einstein field equations in situations where the spacetime is dominated by a known background solution. The technique leverages the knowledge of the background solution to subtract off its contribution to the truncation error, thereby more efficiently achieving a desired level of accuracy. We demonstrate the method by applying it to the radial infall of a solar-type star into supermassive black holes with mass ratios ≥106. The self-gravity of the star is thus consistently modeled within the context of general relativity, and the star's interaction with the black hole computed with moderate computational cost, despite the over five orders of magnitude difference in gravitational potential (as defined by the ratio of mass to radius). We compute the tidal deformation of the star during infall, and the gravitational wave emission, finding the latter is close to the prediction of the point-particle limit.

Original languageEnglish (US)
Article number101502
JournalPhysical Review D - Particles, Fields, Gravitation and Cosmology
Volume87
Issue number10
DOIs
StatePublished - May 16 2013

All Science Journal Classification (ASJC) codes

  • Nuclear and High Energy Physics
  • Physics and Astronomy (miscellaneous)

Fingerprint Dive into the research topics of 'Simulating extreme-mass-ratio systems in full general relativity'. Together they form a unique fingerprint.

Cite this