Authors: Clifford M. Will (Washington University, St. Louis)
Date: 11 Nov 2007
Abstract: If a class of stars orbits the central black hole in our galaxy in short period (~ 0.1 year), high eccentricity (~ 0.9) orbits, they will experience precessions of their orbital planes induced by both relativistic frame-dragging and the quadrupolar gravity of the hole, at levels that could be as large as 10 microarcseconds per year, if the black hole is rotating faster than ½ of its maximum rotation rate. Astrometric observations of the orbits of at least two such stars can in principle lead to a determination of the angular momentum vector J of the black hole and its quadrupole moment Q_2. This could lead to a test of the general relativistic no-hair theorems, which demand that Q_2 = - Jˆ2/M. Future high-precision adaptive infrared optics instruments make make such a fundamental test of the black-hole paradigm possible.
© M. Vallisneri 2012 — last modified on 2010/01/29
Tantum in modicis, quantum in maximis