scholarly journals Understanding the residual patterns of timing solutions of radio pulsars with a model of magnetic field oscillation

2016 ◽  
Vol 459 (1) ◽  
pp. 402-418 ◽  
Author(s):  
Xu-Dong Gao ◽  
Shuang-Nan Zhang ◽  
Shu-Xu Yi ◽  
Yi Xie ◽  
Jian-Ning Fu
Keyword(s):  
Magnetic Field ◽  
Radio Pulsars ◽  
Field Oscillation

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.

Experimental study to control the insertion resistance of internal medical instrument using magnetic field oscillation

2007 ◽  
Vol 40 (2) ◽  
pp. 339-344 ◽  
Author(s):  
K. Yoshinaka ◽  
K. Takashima ◽  
T. Okazaki ◽  
K. Ikeuchi ◽  
T. Washio ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Experimental Study ◽  
Medical Instrument ◽  
Field Oscillation

scholarly journals Pulsars & Magnetars

2008 ◽  
Vol 4 (S259) ◽  
pp. 485-492 ◽  
Author(s):  
Michael Kramer
Keyword(s):  
Magnetic Field ◽  
Neutron Stars ◽  
Evolutionary Sequence ◽  
Radio Pulsars ◽  
Observable Universe ◽  
Spin Evolution ◽  
Field Strengths

AbstractThe largest magnetic field encountered in the observable Universe can be found in neutron stars, in particular in radio pulsars and magnetars. While recent discoveries have slowly started to blur the distinction between these two classes of highly magnetized neutron stars, it is possible that both types of sources are linked via an evolutionary sequence. Indications for this to be the case are obtained from observations of the spin-evolution of pulsars. It is found that most young pulsars are heading across the top of the main distribution of radio pulsars in the P–Ṗ-diagram, suggesting that at least a sub-class of young pulsars may evolve into objects with magnetar-like magnetic field strengths. Part of this evolutionary sequence could be represented by RRATs which appear to share at least in parts properties with both pulsars and magnetars.

scholarly journals LOW-MAGNETIC-FIELD MAGNETARS

2013 ◽  
Vol 22 (13) ◽  
pp. 1330024 ◽  
Author(s):  
ROBERTO TUROLLA ◽  
PAOLO ESPOSITO
Keyword(s):  
Magnetic Field ◽  
Magnetic Energy ◽  
Strong Field ◽  
Radio Pulsars ◽  
X Ray ◽  
Soft Gamma Repeaters ◽  
Dipole Magnetic Field ◽  
Standard Picture ◽  
Observational Status ◽  
Low Magnetic Field

It is now widely accepted that soft gamma repeaters and anomalous X-ray pulsars are the observational manifestations of magnetars, i.e. sources powered by their own magnetic energy. This view was supported by the fact that these "magnetar candidates" exhibited, without exception, a surface dipole magnetic field (as inferred from the spin-down rate) in excess of the electron critical field (≃ 4.4×1013 G). The recent discovery of fully qualified magnetars, SGR 0418+5729 and Swift J1822.3-1606, with dipole magnetic field well in the range of ordinary radio pulsars posed a challenge to the standard picture, showing that a very strong field is not necessary for the onset of magnetar activity (chiefly bursts and outbursts). Here we summarize the observational status of the low-magnetic-field magnetars and discuss their properties in the context of the mainstream magnetar model and its main alternatives.

Magnetic field oscillation in simulations of the Karlsruhe Dynamo

2005 ◽  
Vol 326 (3-4) ◽  
pp. 250-253 ◽  
Author(s):  
A. Sarkar ◽  
A. Tilgner
Keyword(s):  
Magnetic Field ◽  
Field Oscillation

scholarly journals Discovery of Two High Magnetic Field Radio Pulsars

2000 ◽  
Vol 541 (1) ◽  
pp. 367-373 ◽  
Author(s):  
F. Camilo ◽  
V. M. Kaspi ◽  
A. G. Lyne ◽  
R. N. Manchester ◽  
J. F. Bell ◽  
...  
Keyword(s):  
Magnetic Field ◽  
High Magnetic Field ◽  
Radio Pulsars

scholarly journals The velocity distribution of young radio pulsars: simulating the observations

1996 ◽  
Vol 160 ◽  
pp. 53-54 ◽  
Author(s):  
J.W. Hartman
Keyword(s):  
Magnetic Field ◽  
Velocity Distribution ◽  
Proper Motion ◽  
Transverse Velocity ◽  
Radio Pulsar ◽  
Population Synthesis ◽  
Radio Pulsars ◽  
Full Report ◽  
Simulated Sample

Lyne & Lorimer (1994) argue that the velocities of young pulsars are much higher than was previously thought. However, recent radio pulsar population synthesis work by Hartman et al. (1996, these proceedings) shows that simulations that use a birth velocity distribution with more pulsars at low velocities, Phinney’s modification of the Paczyński (1990) distributiondescribes the observed magnetic field, period and luminosity distribution equally well as simulations that use the Lyne & Lorimer distribution.We use this radio pulsar population synthesis model to obtain the proper motion distribution of the simulated sample, and from that we calculate the transverse velocity distribution to compare it with the observed transverse velocity distribution. A full report of this work will be given in Hartman (1996).

scholarly journals Multiphoton amplitude in a constant background field

2018 ◽  
Vol 168 ◽  
pp. 04003
Author(s):  
Aftab Ahmad ◽  
Naser Ahmadiniaz ◽  
Olindo Corradini ◽  
Sang Pyo Kim ◽  
Christian Schubert
Keyword(s):  
Magnetic Field ◽  
Field Theory ◽  
Scattering Amplitude ◽  
Background Field ◽  
Constant Field ◽  
Quantum Field ◽  
Radio Pulsars ◽  
Strong Deviation ◽  
Astrophysical Objects ◽  
Strong External Field

In this contribution, we present our recent compact master formulas for the multiphoton amplitudes of a scalar propagator in a constant background field using the worldline fomulation of quantum field theory. The constant field has been included nonperturbatively, which is crucial for strong external fields. A possible application is the scattering of photons by electrons in a strong magnetic field, a process that has been a subject of great interest since the discovery of astrophysical objects like radio pulsars, which provide evidence that magnetic fields of the order of 1012G are present in nature. The presence of a strong external field leads to a strong deviation from the classical scattering amplitudes. We explicitly work out the Compton scattering amplitude in a magnetic field, which is a process of potential relevance for astrophysics. Our final result is compact and suitable for numerical integration.

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