The Gravitational Wave Signal from Core-collapse Supernovae
Author(s): Morozova, Viktoriya; Radice, David; Burrows, Adam S.; Vartanyan, David
DownloadTo refer to this page use:
http://arks.princeton.edu/ark:/88435/pr1r113
Full metadata record
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Morozova, Viktoriya | - |
dc.contributor.author | Radice, David | - |
dc.contributor.author | Burrows, Adam S. | - |
dc.contributor.author | Vartanyan, David | - |
dc.date.accessioned | 2019-04-10T19:31:40Z | - |
dc.date.available | 2019-04-10T19:31:40Z | - |
dc.date.issued | 2018-07 | en_US |
dc.identifier.citation | Morozova, Viktoriya, Radice, David, Burrows, Adam, Vartanyan, David. (2018). The Gravitational Wave Signal from Core-collapse Supernovae. \apj, 861 (10 - 10. doi:10.3847/1538-4357/aac5f1 | en_US |
dc.identifier.uri | http://arks.princeton.edu/ark:/88435/pr1r113 | - |
dc.description.abstract | We study gravitational waves(GWs)from a set of 2D multigroup neutrino radiation hydrodynamic simulations ofcore-collapse supernovae(CCSNe). Our goal is to systematize the current knowledge about the post-bounce CCSNGW signal and recognize the templatable features that could be used by the ground-based laser interferometers. Wedemonstrate that, starting from∼400 ms after core bounce, the dominant GW signal represents the fundamentalquadrupole(l=2)oscillation mode(f-mode)of the proto–neutron star(PNS), which can be accurately reproducedby a linear perturbation analysis of the angle-averaged PNS profile. Before that, in the time interval between∼200and∼400 ms after bounce, the dominant mode has two radial nodes and represents ag-mode. We associate thehigh-frequency noise in the GW spectrograms above the main signal withp-modes, while below the dominantfrequency there is a region with very little power. The collection of models presented here summarizes thedependence of the CCSN GW signal on the progenitor mass, equation of state, many-body corrections to theneutrino opacity, and rotation. Weak dependence of the dominant GW frequency on the progenitor mass motivatesus to provide a simplefit for it as a function of time, which can be used as a prior when looking for CCSNcandidates in the LIGO data. | en_US |
dc.language.iso | en_US | en_US |
dc.relation.ispartof | Astrophysical Journal | en_US |
dc.rights | Author's manuscript | en_US |
dc.title | The Gravitational Wave Signal from Core-collapse Supernovae | en_US |
dc.type | Journal Article | en_US |
dc.identifier.doi | doi:10.3847/1538-4357/aac5f1 | - |
dc.date.eissued | 2018-06-26 | en_US |
pu.type.symplectic | http://www.symplectic.co.uk/publications/atom-terms/1.0/journal-article | en_US |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
1801.01914.pdf | 13.68 MB | Adobe PDF | View/Download |
Items in OAR@Princeton are protected by copyright, with all rights reserved, unless otherwise indicated.