scholarly journals Are Pulsars Bare Strange Stars?

2000 ◽  
Vol 177 ◽  
pp. 665-666
Author(s):  
R. X. Xu ◽  
G. J. Qiao ◽  
B. Zhang
Keyword(s):  
Magnetic Field ◽  
Neutron Stars ◽  
Strong Magnetic Field ◽  
Strange Star ◽  
Radio Pulsars ◽  
Strong Emission ◽  
Rapid Rotation ◽  
Strange Stars ◽  
Polar Caps ◽  
Supernova Explosions

AbstractIt is believed that pulsars are neutron stars or strange stars with crusts. However we suggest here that pulsars may bebare strange stars(i.e., strange stars without crust). Due to rapid rotation and strong emission, young strange stars produced in supernova explosions should be bare when they act as radio pulsars. Because of strong magnetic field,twopolar-crusts would shield the polar caps of an accreting strange star. Such a suggestion can be checked by further observations.

STRANGE STAR IN THE PRESENCE OF A STRONG MAGNETIC FIELD

2001 ◽  
Vol 16 (13) ◽  
pp. 2435-2445 ◽  
Author(s):  
P. K. SAHU ◽  
S. K. PATRA
Keyword(s):  
Magnetic Field ◽  
Strong Magnetic Field ◽  
Quark Matter ◽  
Strange Star ◽  
Structure Parameters ◽  
Strange Stars ◽  
Strange Matter ◽  
Free Quark ◽  
Star Structure

We study the effect of a strong magnetic field on interacting quark matter and apply the same to strange star. We find that interacting strange matter is less stable than noninteracting strange matter in the presence of a strong magnetic field. We then calculate strange star structure parameters such as mass and radius and find that the strange star is less compact for interacting quark matter than for free quark matter in presence of strong magnetic field. The maximum masses of strange stars are found to be within the recent observational limit.

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 Quadrupole moments of rotating compact stars

2012 ◽  
Vol 8 (S291) ◽  
pp. 536-536
Author(s):  
Martin Urbanec ◽  
John Miller ◽  
Zdenek Stuchlik
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Strange Star ◽  
Compact Stars ◽  
Quadrupole Moments ◽  
Strange Stars

AbstractWe present quadrupole moments of rotating neutron and strange stars calculated using standard Hartle Thorne approach. We demonstrate differences between neutron and strange star parameters connected with quadrupole moments and how this parameters could be, in the case of neutron stars, approximated almost independently on neutron star equation of state.

NEUTRINO ENERGY LOSS ON IRON GROUP NUCLEI BY ELECTRON CAPTURE IN STRONG MAGNETIC FIELD AT THE CRUSTS OF NEUTRON STARS

2007 ◽  
Vol 22 (19) ◽  
pp. 3305-3315 ◽  
Author(s):  
JING-JING LIU ◽  
ZHI-QUAN LUO ◽  
HONG-LIN LIU ◽  
XIANG-JUN LAI
Keyword(s):  
Magnetic Field ◽  
Energy Loss ◽  
Neutron Stars ◽  
Strong Magnetic Field ◽  
Electron Capture ◽  
Neutrino Energy ◽  
Iron Group ◽  
Slight Effect ◽  
The Magnetic Field ◽  
Loss Rates

The neutrino energy loss rates on iron group nuclei by electron capture are calculated in a strong magnetic field at the crusts of Neutron stars. The results show that the magnetic field has only a slight effect on the neutrino energy loss rates in a range of 108–1013 G on surfaces of the most neutron stars. Whereas for some magnetars which range of the magnetic field is 1013–1018 G, the neutrino energy loss rates of the most iron group nuclei would be debased greatly and may be even decreased for 4 orders of magnitude by the strong magnetic field.

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.

Anisotropic cooling and atmospheric radiation of neutron stars with strong magnetic field*

1995 ◽  
Vol 759 (1) ◽  
pp. 291-294 ◽  
Author(s):  
Yu. A. SHIBANOV ◽  
G. G. PAVLOV ◽  
V. E. ZAVLIN ◽  
L. QIN ◽  
S. TSURUTA
Keyword(s):  
Magnetic Field ◽  
Neutron Stars ◽  
Strong Magnetic Field ◽  
Atmospheric Radiation

scholarly journals THE STRONG MAGNETIC FIELD DECAY AND EVOLUTION OF RADIO PULSARS ON THE P–Ṗ DIAGRAM

2004 ◽  
Vol 13 (09) ◽  
pp. 1805-1815 ◽  
Author(s):  
OKTAY H. GUSEINOV ◽  
AŞKIN ANKAY ◽  
SEVINÇ O. TAGIEVA
Keyword(s):  
Magnetic Field ◽  
Observational Data ◽  
Strong Magnetic Field ◽  
Characteristic Time ◽  
Radio Pulsars ◽  
X Ray ◽  
The Real ◽  
Field Decay

In this work we have analysed various data on radio pulsars and we have shown that magnetic field decay of a factor about 10–20 is necessary to explain their evolution, in particular to remove the discrepancy between the characteristic and the real ages. The character of the field decay is exponential with a characteristic time of about 3×106 year. Observational data on single X-ray pulsars which radiate due to cooling also support this result.

scholarly journals Diagnostic of Astrophysical Plasma in Neighborhood of Neutron Stars

1998 ◽  
Vol 188 ◽  
pp. 277-278
Author(s):  
M. Mijatović ◽  
E.A. Solov'ev
Keyword(s):  
Magnetic Field ◽  
Hydrogen Atom ◽  
Neutron Stars ◽  
Strong Magnetic Field ◽  
Astrophysical Plasma ◽  
Hydrogen Atoms ◽  
Astronomical Object

If in the neighborhood of neutron stars exist clouds of hydrogen atoms, they are the natural astronomical object for realization of the model of hydrogen atom in a strong magnetic field ~ 108 T.

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