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Title: Anomalous hydrodynamics kicks neutron stars

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Journal Article: Published Article
Journal Name:
Physics Letters. Section B
Additional Journal Information:
Journal Volume: 760; Journal Issue: C; Related Information: CHORUS Timestamp: 2017-10-28 11:11:07; Journal ID: ISSN 0370-2693
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Citation Formats

Kaminski, Matthias, Uhlemann, Christoph F., Bleicher, Marcus, and Schaffner-Bielich, Jürgen. Anomalous hydrodynamics kicks neutron stars. Netherlands: N. p., 2016. Web. doi:10.1016/j.physletb.2016.06.054.
Kaminski, Matthias, Uhlemann, Christoph F., Bleicher, Marcus, & Schaffner-Bielich, Jürgen. Anomalous hydrodynamics kicks neutron stars. Netherlands. doi:10.1016/j.physletb.2016.06.054.
Kaminski, Matthias, Uhlemann, Christoph F., Bleicher, Marcus, and Schaffner-Bielich, Jürgen. 2016. "Anomalous hydrodynamics kicks neutron stars". Netherlands. doi:10.1016/j.physletb.2016.06.054.
title = {Anomalous hydrodynamics kicks neutron stars},
author = {Kaminski, Matthias and Uhlemann, Christoph F. and Bleicher, Marcus and Schaffner-Bielich, Jürgen},
abstractNote = {},
doi = {10.1016/j.physletb.2016.06.054},
journal = {Physics Letters. Section B},
number = C,
volume = 760,
place = {Netherlands},
year = 2016,
month = 9

Journal Article:
Free Publicly Available Full Text
Publisher's Version of Record at 10.1016/j.physletb.2016.06.054

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Cited by: 11works
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  • The effects of anomalies in high density QCD are striking. We consider a direct application of one of these effects, namely topological currents, on the physics of neutron stars. All the elements required for topological currents are present in neutron stars: degenerate matter, large magnetic fields, and parity violating processes. These conditions lead to the creation of vector currents capable of carrying momentum and inducing magnetic fields. We estimate the size of these currents for many representative states of dense matter in the neutron star and argue that they could be responsible for the large proper motion of neutron starsmore » (kicks), the toroidal magnetic field and finite magnetic helicity needed for stability of the poloidal field, and the resolution of the conflict between type-II superconductivity and precession. Though these observational effects appear unrelated, they likely originate from the same physics — they are all P-odd phenomena that stem from a topological current generated by parity violation.« less
  • We present a newly developed moving-mesh technique for the multi-dimensional Boltzmann-Hydro code for the simulation of core-collapse supernovae (CCSNe). What makes this technique different from others is the fact that it treats not only hydrodynamics but also neutrino transfer in the language of the 3 + 1 formalism of general relativity (GR), making use of the shift vector to specify the time evolution of the coordinate system. This means that the transport part of our code is essentially general relativistic, although in this paper it is applied only to the moving curvilinear coordinates in the flat Minknowski spacetime, since the gravity partmore » is still Newtonian. The numerical aspect of the implementation is also described in detail. Employing the axisymmetric two-dimensional version of the code, we conduct two test computations: oscillations and runaways of proto-neutron star (PNS). We show that our new method works fine, tracking the motions of PNS correctly. We believe that this is a major advancement toward the realistic simulation of CCSNe.« less
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  • The centers of most known galaxies host supermassive black holes (SMBHs). In orbit around these black holes are a centrally concentrated distribution of stars, both in single and in binary systems. Occasionally, these stars are perturbed onto orbits that bring them close to the SMBH. If the star is in a binary system, the three-body interaction with the SMBH can lead to large changes in orbital energy, depositing one of the two stars on a tightly-bound orbit, and its companion into a hyperbolic orbit that may escape the galaxy. In this Letter, we show that the disruption of solitary starsmore » can also lead to large positive increases in orbital energy. The kick velocity depends on the amount of mass the star loses at pericenter, but not on the ratio of black hole to stellar mass, and are at most the star's own escape velocity. We find that these kicks are usually too small to result in the ejection of stars from the Milky Way, but can eject the stars from the black hole's sphere of influence, reducing their probability of being disrupted again. We estimate that {approx} 10{sup 5} stars, {approx} 1% of all stars within 10 pc of the galactic center, are likely to have had mass removed by the central black hole through tidal interaction, and speculate that these 'turbovelocity' stars will at first be redder, but eventually bluer, and always brighter than their unharassed peers.« less
  • This paper describes the steady-state hydrodynamic response of the superfluid interior of a neutron star to the decelerating torque responsible for the slowing-down of pulsars. This torque throws the superfluid into a differential rotation, constant on cylinders but varying with distance from the axis of rotation, plus an exceedingly slow circulation in the r and z directions. This circulation is qualitatively similar to the meridional circulation found in ''ordinary'' stars. The motion of the superfluid does not lead to a tangling of the vortex lines threading it. The superfluid slows at the same rate as the pulsar. (AIP)