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VERSION:2.0
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PRODID:UW-Madison-Physics-Events
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SEQUENCE:3
UID:UW-Physics-Event-6464
DTSTART:20210713T190000Z
DTEND:20210713T200000Z
DTSTAMP:20260414T220205Z
LAST-MODIFIED:20210712T111215Z
LOCATION:https://berkeley.zoom.us/j/91922781599
SUMMARY:Neutrino gravitational wave memory from a core-collapse supern
 ova\, Network in Neutrinos\, Nuclear Astrophysics\, and Symmetries (N3
 AS) Seminar\, Mainak Mukhopadhyay\, Arizona State University
DESCRIPTION:General Relativity predicts that the passage of matter or 
 radiation from an asymmetrically-emitting source should cause a perman
 ent change in the local space-time metric. This phenomenon\, called th
 e \\emph{gravitational memory effect}\, has never been observed\, howe
 ver supernova neutrinos have long been considered a promising avenue f
 or its detection in the future. With the advent of deci-Hertz gravitat
 ional wave interferometers\, observing the  supernova neutrino memory 
 will be possible\, with important implications for multimessenger astr
 onomy and for tests of gravity. In this work\, we develop a phenomenol
 ogical (analytical) toy model for the supernova neutrino memory effect
 \, which is overall consistent with the results of numerical simulatio
 ns. This description is then generalized to several case studies of in
 terest.  We find that\, for a galactic supernova\, the dimensionless s
 train\, $h(t)$\, is of order $\\sim 10^{-22} - 10^{-21}$\, and develop
 s over a typical time scale that varies between $\\sim 0.1 - 10$ s\, d
 epending on the time-evolution of the anisotropy of the neutrino emiss
 ion. The characteristic strain\, $h_c(f)$\, has a maximum at a frequen
 cy $f_{max} \\sim {\\mathcal O}(10^{-1}) - {\\mathcal O}(1)$ Hz. The d
 etailed features of the time- and frequency-structure of the memory st
 rain will inform us of the matter dynamics near the collapsed core\, a
 nd allow to distinguish between different stellar collapse scenarios. 
  Next generation gravitational wave detectors like DECIGO and BBO will
  be sensitive to the neutrino memory effect for supernovae at typical 
 galactic distances and beyond\; with Ultimate DECIGO exceeding a detec
 tability distance of 10 Mpc.  
URL:https://www.physics.wisc.edu/events/?id=6464
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