Gravitational wave signatures of highly compact boson star binaries
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Gravitational wave signatures of highly compact boson star binaries. / Palenzuela, Carlos; Pani, Paolo; Bezares, Miguel; Cardoso, Vitor; Lehner, Luis; Liebling, Steven.
I: Physical Review D, Bind 96, Nr. 10, 104058, 30.11.2017.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Gravitational wave signatures of highly compact boson star binaries
AU - Palenzuela, Carlos
AU - Pani, Paolo
AU - Bezares, Miguel
AU - Cardoso, Vitor
AU - Lehner, Luis
AU - Liebling, Steven
PY - 2017/11/30
Y1 - 2017/11/30
N2 - Solitonic boson stars are stable objects made of a complex scalar field with a compactness that can reach values comparable to that of neutron stars. A recent study of the collision of identical boson stars produced only nonrotating boson stars or black holes, suggesting that rotating boson stars may not form from binary mergers. Here we extend this study to include an analysis of the gravitational waves radiated during the coalescence of such a binary, which is crucial to distinguish these events from other binaries with LIGO and Virgo observations. Our studies reveal that the remnant's gravitational wave signature is mainly governed by its fundamental frequency as it settles down to a nonrotating boson star, emitting significant gravitational radiation during this post-merger state. We calculate how the waveforms and their post-merger frequencies depend on the compactness of the initial boson stars and estimate analytically the amount of energy radiated after the merger.
AB - Solitonic boson stars are stable objects made of a complex scalar field with a compactness that can reach values comparable to that of neutron stars. A recent study of the collision of identical boson stars produced only nonrotating boson stars or black holes, suggesting that rotating boson stars may not form from binary mergers. Here we extend this study to include an analysis of the gravitational waves radiated during the coalescence of such a binary, which is crucial to distinguish these events from other binaries with LIGO and Virgo observations. Our studies reveal that the remnant's gravitational wave signature is mainly governed by its fundamental frequency as it settles down to a nonrotating boson star, emitting significant gravitational radiation during this post-merger state. We calculate how the waveforms and their post-merger frequencies depend on the compactness of the initial boson stars and estimate analytically the amount of energy radiated after the merger.
KW - BLACK-HOLES
KW - RELATIVITY
U2 - 10.1103/PhysRevD.96.104058
DO - 10.1103/PhysRevD.96.104058
M3 - Journal article
VL - 96
JO - Physical Review D
JF - Physical Review D
SN - 2470-0010
IS - 10
M1 - 104058
ER -
ID: 299401057