scholarly journals The influence of magnetic field geometry in neutron stars' crustal oscillations

2019 ◽  
Vol 340 (9-10) ◽  
pp. 904-908
Author(s):  
Gibran H. Souza ◽  
Ernesto Kemp
Keyword(s):  
Magnetic Field ◽  
Neutron Stars ◽  
Field Geometry

scholarly journals Starquakes in Neutron Stars

2000 ◽  
Vol 195 ◽  
pp. 391-392
Author(s):  
L. M. Franco ◽  
B. Link ◽  
R. I. Epstein
Keyword(s):  
Magnetic Field ◽  
Angular Momentum ◽  
Neutron Star ◽  
Neutron Stars ◽  
External Torque ◽  
Field Geometry ◽  
Magnetic Poles ◽  
Asymmetric Matter ◽  
The Magnetic Field ◽  
Permanent Increase

The Crab and other pulsars suffer sudden and permanent increases in their spin-down rates in association with glitches, suggesting that the external torque on these objects grows in steps. Here, we describe how torque changes may arise from starquakes, occurring as the star spins down and its rigid crust becomes less oblate. We study the evolution of strain in the crust, the initiation of starquakes, the effects on the magnetic field geometry, and possible observable consequences for neutron star spin down. We find that the stellar crust begins breaking at the rotational equator, forming a fault inclined at an angle to the equator and directed toward the magnetic poles. The resulting asymmetric matter redistribution produces a misalignment of the angular momentum and spin axes. Subsequently, damped precession to a new rotational state increases the angle between rotation and magnetic axes. The change in this angle could increase the external torque, producing a permanent increase in the spin-down rate.

scholarly journals A New View on Young Pulsars in Supernova Remnants: Slow, Radio-quiet & X-ray Bright

2000 ◽  
Vol 177 ◽  
pp. 699-702 ◽  
Author(s):  
E. V. Gotthelf ◽  
G. Vasisht
Keyword(s):  
Magnetic Field ◽  
Neutron Stars ◽  
Supernova Remnants ◽  
Simple Explanation ◽  
Crab Pulsar ◽  
Radio Pulsars ◽  
Substantial Fraction ◽  
Subsequent Evolution ◽  
X Ray ◽  
Field Decay

AbstractWe propose a simple explanation for the apparent dearth of radio pulsars associated with young supernova remnants (SNRs). Recent X-ray observations of young remnants have revealed slowly rotating (P∼ 10s) central pulsars with pulsed emission above 2 keV, lacking in detectable radio emission. Some of these objects apparently have enormous magnetic fields, evolving in a manner distinct from the Crab pulsar. We argue that these X-ray pulsars can account for a substantial fraction of the long sought after neutron stars in SNRs and that Crab-like pulsars are perhaps the rarer, but more highly visible example of these stellar embers. Magnetic field decay likely accounts for their high X-ray luminosity, which cannot be explained as rotational energy loss, as for the Crab-like pulsars. We suggest that the natal magnetic field strength of these objects control their subsequent evolution. There are currently almost a dozen slow X-ray pulsars associated with young SNRs. Remarkably, these objects, taken together, represent at least half of the confirmed pulsars in supernova remnants. This being the case, these pulsars must be the progenitors of a vast population of previously unrecognized neutron stars.

scholarly journals Magnetic field amplification in newly-born neutron stars

1996 ◽  
Vol 160 ◽  
pp. 435-436
Author(s):  
H.-J. Wiebicke ◽  
U. Geppert
Keyword(s):  
Magnetic Field ◽  
Neutron Stars ◽  
Gravitational Collapse ◽  
Dipole Field ◽  
Numerical Calculations ◽  
Selection Effects ◽  
Thermoelectric Effects ◽  
Field Amplification ◽  
Seed Field ◽  
Flux Conservation

AbstractWe present a scenario of magnetic field (MF) evolution of newly-born neutron stars (NSs). Numerical calculations show that in the hot phase of young NSs the MF can be amplified by thermoelectric effects, starting from a moderately strong seed-field. Therefore, there is no need to assume a 1012G dipole field immediately after the gravitational collapse of the supernova (SN) event. The widely accepted scenario for such a field to be produced by flux conservation during the collapse is critically discussed. Instead, it can be generated by amplification and selection effects in the first 104yrs, and by the subsequent fast ohmic decay of higher multipole components, when the NS cools down.

Jupiter's internal magnetic field geometry relevant to particle trapping

1977 ◽  
Vol 82 (32) ◽  
pp. 5187-5194 ◽  
Author(s):  
Juan G. Roederer ◽  
Mario H. Acuña ◽  
Norman F. Ness
Keyword(s):  
Magnetic Field ◽  
Internal Magnetic Field ◽  
Particle Trapping ◽  
Field Geometry

scholarly journals Could a change in magnetic field geometry cause the break in the wind-activity relation?

2015 ◽  
Vol 455 (1) ◽  
pp. L52-L56 ◽  
Author(s):  
A. A. Vidotto ◽  
J.-F. Donati ◽  
M. Jardine ◽  
V. See ◽  
P. Petit ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Field Geometry ◽  
Wind Activity

scholarly journals Evidence for Heating of Neutron Stars by Magnetic-Field Decay

2007 ◽  
Vol 98 (7) ◽  
Author(s):  
José A. Pons ◽  
Bennett Link ◽  
Juan A. Miralles ◽  
Ulrich Geppert
Keyword(s):  
Magnetic Field ◽  
Neutron Stars ◽  
Field Decay

scholarly journals Mutual influence of magnetic field decay and thermal evolution of rotational neutron stars

2012 ◽  
Vol 8 (S291) ◽  
pp. 586-588
Author(s):  
Xia Zhou ◽  
Miao Kang ◽  
Na Wang
Keyword(s):  
Magnetic Field ◽  
Neutron Stars ◽  
Mutual Influence ◽  
Thermal Evolution ◽  
Chemical Heating ◽  
Field Decay ◽  
The Magnetic Field

AbstractThe effect of magnetic field decay on the chemical heating and thermal evolution of neutron stars is discussed. Our main goal is to study how chemical heating mechanisms and thermal evolution are changed by field decay and how magnetic field decay is modified by the thermal evolution. We show that the effect of chemical heating is suppressed by the star spin-down through decaying magnetic field at a later stage; magnetic field decay is delayed significantly relative to stars cooling without heating mechanisms; compared to typical chemical heating, the decay of the magnetic field can even cause the temperature to turn down at a later stage.

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