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Study of Binary Black Hole Dynamics ...

McCammon, Cody,

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Study of Binary Black Hole Dynamics Using Gravitational Waves /

Record Type:	Electronic resources : Monograph/item
Title/Author:	Study of Binary Black Hole Dynamics Using Gravitational Waves // Cody McCammon.
Author:	McCammon, Cody,
Description:	1 electronic resource (41 pages)
Notes:	Source: Masters Abstracts International, Volume: 86-03.
Contained By:	Masters Abstracts International86-03.
Subject:	Astrophysics. -
Online resource:	https://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=31490033
ISBN:	9798384437154

Study of Binary Black Hole Dynamics Using Gravitational Waves /
McCammon, Cody,

Study of Binary Black Hole Dynamics Using Gravitational Waves /Cody McCammon. - 1 electronic resource (41 pages)

Source: Masters Abstracts International, Volume: 86-03.

Merging binary black holes exhibit precessional motion that can be classified into three distinct morphologies: Circulating, librating around 0, and librating around π. This information is decoded from the gravitational wave signal. Binary systems can transition between morphologies as they spiral inwards, and spin precession effects are more pronounced near merger. The spin morphology reveals information about the binary black holes' formation such as through isolated evolution of massive binary stars and their collapse or through dynamic evolution channels such as capture. In this study, we considered inferring the morphology at reference points at which the binary has (approximately) a given orbital velocity using both dimensionless frequency corresponding to 20 Hz and dimensionless time corresponding to t = −100M. Previous studies have instead used a reference point at a given gravitational wave frequency, which corresponds to different orbital velocities depending on the binary's properties. We simulated loud gravitational wave signals from spinning binary black holes in the LIGO-Virgo network at its plus-era sensitivity and constrained their precessional morphologies. We then compared the results to those from previous work to see if there are better constraints at these new reference points. We find that one can obtain both better and worse constraints at a fixed orbital velocity than at a fixed gravitational wave frequency. This study helps determine a suitable reference point for constraining binary black hole spin morphologies.

English

ISBN: 9798384437154Subjects--Topical Terms:

535904
Astrophysics.
Subjects--Index Terms:

Spin morphology

Study of Binary Black Hole Dynamics Using Gravitational Waves /
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245 1 0 $a Study of Binary Black Hole Dynamics Using Gravitational Waves / $c Cody McCammon.
264 1 $a Ann Arbor : $b ProQuest Dissertations & Theses, $c 2024
300 $a 1 electronic resource (41 pages)
336 $a text $b txt $2 rdacontent
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500 $a Source: Masters Abstracts International, Volume: 86-03.
500 $a Advisors: Gupta, Anuradha Committee members: MacDonald, Nicholas; Davies, Gavin.
502 $b M.S. $c The University of Mississippi $d 2024.
520 $a Merging binary black holes exhibit precessional motion that can be classified into three distinct morphologies: Circulating, librating around 0, and librating around π. This information is decoded from the gravitational wave signal. Binary systems can transition between morphologies as they spiral inwards, and spin precession effects are more pronounced near merger. The spin morphology reveals information about the binary black holes' formation such as through isolated evolution of massive binary stars and their collapse or through dynamic evolution channels such as capture. In this study, we considered inferring the morphology at reference points at which the binary has (approximately) a given orbital velocity using both dimensionless frequency corresponding to 20 Hz and dimensionless time corresponding to t = −100M. Previous studies have instead used a reference point at a given gravitational wave frequency, which corresponds to different orbital velocities depending on the binary's properties. We simulated loud gravitational wave signals from spinning binary black holes in the LIGO-Virgo network at its plus-era sensitivity and constrained their precessional morphologies. We then compared the results to those from previous work to see if there are better constraints at these new reference points. We find that one can obtain both better and worse constraints at a fixed orbital velocity than at a fixed gravitational wave frequency. This study helps determine a suitable reference point for constraining binary black hole spin morphologies.
546 $a English
590 $a School code: 0131
650 4 $a Astrophysics. $3 535904
650 4 $a Physics. $3 516296
650 4 $a Astronomy. $3 517668
653 $a Spin morphology
653 $a Virgo network
653 $a Black holes
690 $a 0596
690 $a 0606
690 $a 0605
710 2 $a The University of Mississippi. $b Physics. $e degree granting institution. $3 3816213
720 1 $a Gupta, Anuradha $e degree supervisor.
773 0 $t Masters Abstracts International $g 86-03.
790 $a 0131
791 $a M.S.
792 $a 2024
856 4 0 $u https://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=31490033