Gravitational waves from neutron stars and asteroseismology
Gravitational waves from neutron stars and asteroseismology
Neutron stars are born in the supernova explosion of massive stars. Neutron stars rotate as stably as atomic clocks and possess densities exceeding that of atomic nuclei and magnetic fields millions to billions of times stronger than those created in laboratories on Earth. The physical properties of neutron stars are determined by many areas of fundamental physics, and detection of gravitational waves can provide invaluable insights into our understanding of these areas. Here we describe some of the physics and astrophysics of neutron stars and how traditional electromagnetic wave observations provide clues to the sorts of gravitational waves we expect from these stars. We pay particular attention to neutron star fluid oscillations, examining their impact on electromagnetic and gravitational wave observations when these stars are in a wide binary or isolated system, then during binary inspiral right before merger, and finally at times soon after merger.
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Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
28 May 2018
Ho, Wynn C.G.
d78d4c52-8f92-4846-876f-e04a8f803a45
Ho, Wynn C.G.
(2018)
Gravitational waves from neutron stars and asteroseismology.
Philosophical Transactions of The Royal Society A, 376 (2120), , [20170285].
(doi:10.1098/rsta.2017.0285).
Abstract
Neutron stars are born in the supernova explosion of massive stars. Neutron stars rotate as stably as atomic clocks and possess densities exceeding that of atomic nuclei and magnetic fields millions to billions of times stronger than those created in laboratories on Earth. The physical properties of neutron stars are determined by many areas of fundamental physics, and detection of gravitational waves can provide invaluable insights into our understanding of these areas. Here we describe some of the physics and astrophysics of neutron stars and how traditional electromagnetic wave observations provide clues to the sorts of gravitational waves we expect from these stars. We pay particular attention to neutron star fluid oscillations, examining their impact on electromagnetic and gravitational wave observations when these stars are in a wide binary or isolated system, then during binary inspiral right before merger, and finally at times soon after merger.
Text
ho17v2
- Accepted Manuscript
More information
Accepted/In Press date: 8 January 2018
e-pub ahead of print date: 16 April 2018
Published date: 28 May 2018
Identifiers
Local EPrints ID: 416875
URI: http://eprints.soton.ac.uk/id/eprint/416875
ISSN: 1364-503X
PURE UUID: 859740ec-8405-4d88-a4c8-76fd06e53d19
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Date deposited: 12 Jan 2018 17:30
Last modified: 16 Mar 2024 06:06
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