Magnetic Field Evolution in Neutron Star Crusts Due to the Hall Effect and Ohmic Decay
By A. Cumming, Philipp Arras, E. Zweibel. 2004
182 citations recorded by the source corpus.
We present calculations of magnetic field evolution by the Hall effect and ohmic decay in the crust of neutron stars (NSs). In accreting NSs, ohmic decay is always the dominant effect because of the large resistivity. In isolated NSs with relatively pure crusts, the Hall effect dominates ohmic decay after a time tswitch ≃ 104 yr B, where B12 is the magnetic field strength in units of 1012 G. We compute the evolution of an initial field distribution by ohmic decay and give approximate analytic formulae for both the surface and interior fields as a function of time. Because of the strong dependence of tswitch on B12, early ohmic decay can alter the currents down to the base of the crust for B ~ 1011 G, neutron drip for B ~ 1012 G, and near the top of the crust for B ≳ 1013 G. We then discuss magnetic field evolution by the Hall effect. Several examples are given to illustrate how an initial field configuration evolves. Hall-wave eigenfunctions are computed, including the effect of the large density change across the crust. We estimate the response of the crust to the magnetic stresses induced by Hall waves and give a detailed discussion of the boundary conditions at the solid-liquid interface. Finally, we discuss the implications for the Hall cascade proposed by Goldreich & Reisenegger.
Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Geophysics
View Paper: https://www.semanticscholar.org/paper/b18e42546ee6a5c19965c0067056981829cc1e96
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Citations in the corpus
- Physics of strongly magnetized neutron stars (2006, background): “Of course, currents which are confined to the crust would have a much shorter decay time (e.g. Sang and Chanmugam (1987), Cumming et al (2004)).”
- Wave turbulence in incompressible Hall magnetohydrodynamics (2006, background): “The importance of the Hall effect in astrophysics has been pointed out to understand, for example, the presence of instabilities in protostellar disks (Balbus and Terquem 2001), the magnetic field evolution in neutron star crusts (Goldreich and Reisenegger 1992; Cumming et al. 2004), impulsive magne”
- Magnetic field dissipation in neutron star crusts: From magnetars to isolated neutron stars (2007, background): “…et al. 1990; Goldreich & Reisenegger 1992; Muslimov 1994; Naito & Kojima 1994; Urpin & Shalybkov 1995; Shalybkov & Urpin 1997; Vainshtein et al. 2000; Rheinhardt & Geppert 2002; Geppert & Rheinhardt 2002; Hollerbach & Ruediger 2002; Geppert et al. 2003; Rheinhardt et al. 2004; Cumming et al. 2004).”
- Unifying the observational diversity of isolated neutron stars via magneto-thermal evolution models. (2013, background): “The evolution of the magnetic field in NSs has been studied extensively by a number of authors (Goldreich & Reisenegger 1992; Geppert & Rheinhardt 2002; Hollerbach & Rüdiger 2002, 2004; Cumming et al. 2004; Arras et al. 2004; Pons et al. 2007; Gonzalez & Reisenegger 2010; Glampedakis et al. 2011).”
- Gravitational Radiation from an Accreting Millisecond Pulsar with a Magnetically Confined Mountain (2005, background): “The timescale of this process is sensitive to the field geometry (as well as the radial profiles of the electron density and elastic shear modulus in the crust) (Cumming et al. 2004); it will be interesting to evaluate it for the distorted field produced by magnetic burial.”