On the electron cap shape of a rotating neutron star with a strong magnetic field

1977 ◽  
Vol 51 (1) ◽  
pp. 59-75 ◽  
Author(s):  
Yu. A. Rylov
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Strong Magnetic Field

scholarly journals The Gravitomagnetic Effects in Rapidly Rotating Neutron Stars: A Theoretical Study

2020 ◽  
Vol 2 (2) ◽  
pp. 149-157
Author(s):  
Atsnaita Yasrina ◽  
Nugroho Adi Pramono
Keyword(s):  
Magnetic Field ◽  
Gravitational Field ◽  
Neutron Star ◽  
Neutron Stars ◽  
Strong Magnetic Field ◽  
Rotational Speed ◽  
Distribution Density ◽  
Theoretical Study ◽  
Electromagnetic Measurements ◽  
General Relativistic

Electromagnetic measurements of a general relativistic gravitomagnetic effect can be done within the conductor embedded in a rotating gravitational object’s spacetime. Neutron stars are rotating gravitational object that have strong magnetic field. The gravitomagnetic effect in a neutron star can be determined from the distribution density in the conductor. Neutron star is assumed as a conductor and it rotates rapidly. The distribution density inside the conductor is obtained from the electromagnetic contravariant tensor and the relativistic rotational speed of the conductor. It has obtained the distribution density inside the conductor for the rapidly rotating neutron star. The results are compared to the slowly rotating neutron star which depends on the angular veolocity and the gravitational field.

Photon splitting in the strong magnetic field of a neutron star

2000 ◽  
Vol 19 (3-4) ◽  
pp. 485-494
Author(s):  
E. V. Derishev ◽  
V. V. Kocharovsky ◽  
VI. V. Kocharovsky
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Strong Magnetic Field ◽  
Photon Splitting

PROTON BRANCH OF MODIFIED URCA PROCESS IN STRONG MAGNETIC FIELD AND SUPERFLUIDITY OF NEUTRON STAR CORES

2010 ◽  
Vol 19 (03) ◽  
pp. 437-447 ◽  
Author(s):  
JIE ZHANG ◽  
SHAO-FENG WANG ◽  
MEN-QUAN LIU
Keyword(s):  
Magnetic Field ◽  
Critical Temperature ◽  
Neutron Star ◽  
Strong Magnetic Field ◽  
Chemical Potential ◽  
Neutrino Energy ◽  
Zero Magnetic Field ◽  
Initial Stage ◽  
Neutron Star Cooling ◽  
Urca Process

The modified URCA process produces efficient neutrino energy losses in neutron star cores, and has been shown to go via neutron and proton branches. Based on the improved electron chemical potential and critical temperature of superfluidity, the effects of strong magnetic field and superfluidity on the proton branch of modified URCA process are investigated simultaneously in this paper. The results show that strong magnetic field enhances the neutrino emissivities compared to the case in zero magnetic field, and superfluidity reduces the emissivities significantly. For the total neutrino emissivities, the magnetic field is dominant at the initial stage of neutron star cooling, but the superfluidity becomes crucial as the temperature drops below the critical temperature.

scholarly journals Reverse shocks in the relativistic outflows of gravitational wave-detected neutron star binary mergers

2019 ◽  
Vol 489 (2) ◽  
pp. 1820-1827 ◽  
Author(s):  
Gavin P Lamb ◽  
Shiho Kobayashi
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Gravitational Wave ◽  
Strong Magnetic Field ◽  
Gamma Ray ◽  
Reverse Shock ◽  
Central Engine ◽  
Forward Shock ◽  
Binary Mergers ◽  
Star Binary

ABSTRACT The afterglows to gamma-ray bursts (GRBs) are due to synchrotron emission from shocks generated as an ultrarelativistic outflow decelerates. A forward and a reverse shock will form, however, where emission from the forward shock is well studied as a potential counterpart to gravitational wave-detected neutron star mergers the reverse shock has been neglected. Here, we show how the reverse shock contributes to the afterglow from an off-axis and structured outflow. The off-axis reverse shock will appear as a brightening feature in the rising afterglow at radio frequencies. For bursts at ∼100 Mpc, the system should be inclined ≲20° for the reverse shock to be observable at ∼0.1–10 d post-merger. For structured outflows, enhancement of the reverse shock emission by a strong magnetic field within the outflow is required for the emission to dominate the afterglow at early times. Early radio photometry of the afterglow could reveal the presence of a strong magnetic field associated with the central engine.

scholarly journals Radio emission from the X-ray pulsar Her X-1: a jet launched by a strong magnetic field neutron star?

2017 ◽  
Vol 473 (1) ◽  
pp. L141-L145 ◽  
Author(s):  
J van den Eijnden ◽  
N Degenaar ◽  
T D Russell ◽  
J C A Miller-Jones ◽  
R Wijnands ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Radio Emission ◽  
Strong Magnetic Field ◽  
X Ray

scholarly journals Deformation of neutron stars due to poloidal magnetic fields

2019 ◽  
Vol 2019 (8) ◽  
Author(s):  
K Yanase ◽  
N Yoshinaga ◽  
E Nakano ◽  
C Watanabe
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Magnetic Fields ◽  
Neutron Stars ◽  
Strong Magnetic Field ◽  
Axially Symmetric ◽  
Poloidal Magnetic Field ◽  
The One ◽  
Poloidal Magnetic Fields

Abstract The mass–radius (MR) relation of deformed neutron stars in the axially symmetric poloidal magnetic field is calculated. The MR relation is obtained by solving the Hartle equations, whereas the one for spherical stars is obtained by the Tolman–Oppenheimer–Volkoff equations. The anisotropic effects of the poloidal magnetic fields are found to be non-negligible for a strong magnetic field more than $3\times10^{18}$ G at the center of a neutron star.

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