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SUMMARY:Finding self-force quantities in a post-Newtonian expansion: Eccen
tric orbits on a Schwarzschild background
DTSTART;VALUE=DATE-TIME:20151112T104500Z
DTEND;VALUE=DATE-TIME:20151112T114500Z
DTSTAMP;VALUE=DATE-TIME:20190821T140836Z
UID:indico-event-906@indico.math.cnrs.fr
DESCRIPTION:Small compact objects orbiting supermassive back holes are an
important potential source of gravitational radiation. Detection of such w
aves and the parameter estimation of their sources will require accurate w
aveform templates. To this eventual end\, I present work on bound eccentri
c motion around a static black hole. In two separate approaches\, I examin
e solutions to the first order (in mass-ratio) field equations. First\, I
consider solving the field equations entirely analytically in a double pos
t-Newtonian/small-eccentricity expansion. Then I show numeric work wherein
we use the MST formalism to solve the field equations to 200 digits. We u
se this extreme accuracy to fit for previously unknown PN energy flux para
meters\, extending the previous state of the art from 3PN to 7PN.\n\nhttps
://indico.math.cnrs.fr/event/906/
LOCATION:IHES Amphithéâtre Léon Motchane
URL:https://indico.math.cnrs.fr/event/906/
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