The Soft Gamma Repeaters as Very Strongly Magnetized Neutron Stars. II. Quiescent Neutrino, X-Ray, and Alfvén Wave Emission
Reads0
Chats0
TLDR
In this article, the decay rate of the core field is a very strong function of temperature and therefore of the magnetic flux density, which is not present in the decay of the weaker fields associated with ordinary radio pulsars.Abstract:
We calculate the quiescent X-ray, neutrino, and Alfven wave emission from a neutron star with a very strong magnetic field, Bdipole ~ 1014 − 1015 G and Binterior ~ (5–10) × 1015 G. These results are compared with observations of quiescent emission from the soft gamma repeaters and from a small class of anomalous X-ray pulsars that we have previously identified with such objects. The magnetic field, rather than rotation, provides the main source of free energy, and the decaying field is capable of powering the quiescent X-ray emission and particle emission observed from these sources. New features that are not present in the decay of the weaker fields associated with ordinary radio pulsars include fracturing of the neutron star crust, strong heating of its core, and effective suppression of thermal conduction perpendicular to the magnetic field. As the magnetic field is forced through the crust by diffusive motions in the core, multiple small-scale fractures are excited, as well as a few large fractures that can power soft gamma repeater bursts. The decay rate of the core field is a very strong function of temperature and therefore of the magnetic flux density. The strongest prediction of the model is that these sources will show no optical emissions associated with X-ray heating of an accretion disk.read more
Citations
More filters
Journal ArticleDOI
The Australia Telescope National Facility Pulsar Catalogue
TL;DR: A new and complete catalog of the main properties of the 1509 pulsars for which published information currently exists, which includes all spin-powered pulsars, as well as anomalous X-ray pulsars and soft gamma-ray repeaters showing coherent pulsed emission.
Journal ArticleDOI
Neutron star observations: Prognosis for equation of state constraints
TL;DR: In this article, the authors investigate how current and proposed observations of neutron stars can lead to an understanding of the state of their interiors and the key unknowns: the typical neutron star radius and the neutron star maximum mass.
Journal ArticleDOI
An X-ray pulsar with a superstrong magnetic field in the soft γ-ray repeater SGR1806 − 20
Chryssa Kouveliotou,Chryssa Kouveliotou,S. Dieters,S. Dieters,Tod E. Strohmayer,Tod E. Strohmayer,J. van Paradijs,Gerald J. Fishman,Charles A. Meegan,Kevin Hurley,Jefferson M. Kommers,Ian Smith,Dale A. Frail,Toshio Murakami +13 more
TL;DR: In this paper, the authors reported the discovery of pulsations in the persistent X-ray flux of SGR1806-20, with a period of 7.47 s and a spindown rate of 2.6 x 10(exp -3) s/yr.
Journal ArticleDOI
Neutron Star Observations: Prognosis for Equation of State Constraints
TL;DR: In this article, a theoretical analysis of neutron star structure, including general relativistic limits to mass, compactness, and spin rates, is presented. But the authors focus on the state of the interiors and the key unknowns: the typical neutron star radius and the maximum mass.
Journal ArticleDOI
Gamma-Ray Bursts: Progress, Problems & Prospects
Bing Zhang,Peter Mészáros +1 more
TL;DR: The cosmological gamma-ray burst (GRB) phenomenon is reviewed in this article, where broad observational facts and empirical phenomenological relations of the GRB prompt emission and afterglow are outlined.
References
More filters
MonographDOI
Black Holes, White Dwarfs, and Neutron Stars
TL;DR: In this paper, the soft file of a book collection of black holes white dwarfs and neutron stars can be downloaded and the book can be found on-line in this site.
Journal ArticleDOI
Formation of very strongly magnetized neutron stars - Implications for gamma-ray bursts
TL;DR: In this article, it is argued that a convective dynamo can also generate a very strong dipole field after the merger of a neutron star binary, but only if the merged star survives for as long as about 10-100 ms.
Journal ArticleDOI
The soft gamma repeaters as very strongly magnetized neutron stars - I. Radiative mechanism for outbursts
Journal ArticleDOI
Neutron star dynamos and the origins of pulsar magnetism
TL;DR: In this article, it is argued that most of the magnetic energy becomes concentrated in thin flux ropes when the field pressure exceeds the turbulent pressure at the smallest scale of turbulence, and the possibilities for dynamo action during the various (precollapse) stages of convective motion that occur in the evolution of a massive star are examined.
Journal ArticleDOI
Magnetic field decay in isolated neutron stars
TL;DR: In this article, the authors investigated three mechanisms that promote the loss of magnetic flux from an isolated neutron star, including buoyant rise and dragging by superfluid neutron vectors, and found that the drift speed is proportional to the second power of the magnetic field strength.