Modelling magnetically deformed neutron stars

By Brynmor Haskell, L. Samuelsson, K. Glampedakis, N. Andersson. 2007

158 citations recorded by the source corpus.

Rotating deformed neutron stars are important potential sources for ground-based gravitational wave interferometers such as LIGO, GEO600 and VIRGO. One mechanism that may lead to significant non-asymmetries is the internal magnetic field. It is well known that a magnetic star will not be spherical and, if the magnetic axis is not aligned with the spin axis, the deformation will lead to the emission of gravitational waves. The aim of this paper is to develop a formalism that would allow us to model magnetically deformed stars, using both realistic equations of state and field configurations. As a first step, we consider a set of simplified model problems. Focusing on dipolar fields, we determine the internal magnetic field which is consistent with a given neutron star model and calculate the associated deformation. We discuss the relevance of our results for current gravitational wave detectors and future prospects.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/d7cff14439ea668453b9596eccc9fd9c7d235d66

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. P. Lasky
2. Kent Yagi
3. N. Yunes
4. C. Berry
5. Christopher J. Moore
6. Robert H. Cole
7. A. Watts
8. Bernard F. Schutz

In Atomic and Molecular Physics, and Optics

1. Bernard F. Schutz
2. N. Yunes
3. P. Lasky
4. B. Krishnan
5. L. Bildsten
6. Kent Yagi
7. A. Watts

In Ocean Engineering

1. Bernard F. Schutz
2. N. Yunes
3. P. Lasky
4. L. Bildsten
5. Kent Yagi
6. A. Watts
7. Luciano Rezzolla
8. C. Breu

Citations in the corpus

• Detecting gravitational wave emission from the known accreting neutron stars (2008, background): “…Ushomirsky, Cutler & Bildsten 2000; Melatos & Payne 2005; Payne & Melatos 2006; Haskell, Jones & Andersson 2006), magnetic deformation (Cutler 2002; Haskell et al. 2008) or internal r-mode oscillations (Bildsten 1998; Andersson, Kokkotas & Stergioulas 1999; Levin 1999; Andersson et al. 2000; Heyl…”
• The birth of black holes: neutron star collapse times, gamma-ray bursts and fast radio bursts (2014, background): “Magnetic field-induced deformities are not expected to cause significant GW emission over longer time-scales (Haskell et al. 2008).”
• Approximate Universal Relations for Neutron Stars and Quark Stars (2016, background): “[189] in the Newtonian limit, the I-Q relation for magnetized Newtonian stars with an n = 1 polytropic equation of state is approximately [53]”
• Gravitational Waves from Neutron Stars: A Review (2015, background): “The relative strengths of poloidal and toroidal components strongly affects the stellar ellipticity, and hence gravitational wave detectability (Haskell et al. 2008; Colaiuda et al. 2008; Ciolfi et al. 2009; Mastrano et al. 2011).”
• Gravitational-wave sensitivity curves (2014, background): “e neutron star equation of state and the stiness of the crust, which are currently uncertain (Chamel and Haensel, 2008; Lattimer, 2012). Deformations can also be supported by internal magnetic elds (Haskell et al., 2008). Several known pulsars could be sources for the advanced detectors and upper li”