scholarly journals On Possible Reduction of Equilibrium Radius of a Neutron Star Influenced by Superstrong Magnetic Field

2012 ◽  
Vol 2012 ◽  
pp. 1-6
Author(s):  
Vladimir V. Skobelev
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Electron Gas ◽  
Necessary Condition ◽  
Superstrong Magnetic Field ◽  
Stellar Objects ◽  
New Class ◽  
Short Period ◽  
Equilibrium Radius ◽  
Field Influence

Necessary condition forβ-decay suppression of a neutron in degenerate magnetized electron gas is formulated. Based on this, it is shown that, in superstrong magnetic field, equilibrium radius of a neutron star is approximately several times smaller than without the field influence. Therefore, we can make a prediction that in short-period pulsars, such fields can be observed. In fact, possible existence of new class of stellar objects is noted, the objects with superstrong magnetic field and supersmall radius about 1 km which we namedminimagnetars. They can be detected by gravitational red shift of their radiation.

scholarly journals Concept of Gravito-Rotational Acceleration and its Consequences for Compact Stellar Objects

2021 ◽  
Author(s):  
Mohamed Hassani
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Equation Of State ◽  
Orbital Motion ◽  
Rotational Acceleration ◽  
Material Body ◽  
Stellar Objects ◽  
Gravitational Action ◽  
Theories Of Gravity ◽  
Previous Series

In a previous series of papers relating to the Combined Gravitational Action (CGA), we have exclusively studied orbital motion without spin. In the present paper, we apply CGA to any self-rotating material body, i.e., an axially spinning massive object, which itself may be locally seen as a gravito-rotational source because it is capable of generating the gravito-rotational acceleration, which seems to be unknown to previously existing theories of gravity. The consequences of such an acceleration are very interesting, particularly for Compact Stellar Objects. Independently of the equation of state, it is found that the critical and maximum internal magnetic field strength of a stable neutron star cannot exceed the value of 3x1018G.

scholarly journals On the Concept of Gravito-Rotational Acceleration and its Consequences for Compact Stellar Objects

2021 ◽  
Author(s):  
Mohamed Elmansour Hassani
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Orbital Motion ◽  
Rotational Acceleration ◽  
Gravitational Radius ◽  
Material Body ◽  
Stellar Objects ◽  
Gravitational Action ◽  
Theories Of Gravity ◽  
Previous Series

In a previous series of papers relating to the Combined Gravitational Action (CGA), we have exclusively studied orbital motion without spin. In the present paper, we apply CGA to any self-rotating material body, i.e., an axially spinning massive object, which itself may be locally seen as a gravito-rotational source because it is capable of generating the gravito-rotational acceleration, which seems to be unknown to previously existing theories of gravity. The consequences of such an acceleration are very interesting, particularly for Compact Stellar Objects. Independently of the equation of state, it is found that the minimum radius of a stable neutron star is three times its gravitational radius, Rmin = 3GMNS/c2, and its critical and maximum internal magnetic field strength cannot exceed the value of 3×1018 G.

Physical Interpretations of Internal Magnetic Field Influence on Processes in Tribocontact of Textured Dimple Surfaces

2019 ◽  
Vol 11 (5) ◽  
pp. 05013-1-05013-5
Author(s):  
V. Ye. Marchuk ◽  
◽  
M. V. Kindrachuk ◽  
V. I. Mirnenko ◽  
R. G. Mnatsakanov ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Internal Magnetic Field ◽  
Field Influence

scholarly journals Effect of magnetic field on the burning of a neutron star

2018 ◽  
Vol 27 (10) ◽  
pp. 1850083 ◽  
Author(s):  
Ritam Mallick ◽  
Amit Singh
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Initial Density ◽  
Considerable Effect ◽  
Magnetic Axis ◽  
Small Window ◽  
Exothermic Process ◽  
Text Density ◽  
The Magnetic Field ◽  
Observational Aspect

In this paper, we present the effect of a strong magnetic field in the burning of a neutron star (NS). We have used relativistic magneto-hydrostatic (MHS) conservation equations for studying the PT from nuclear matter (NM) to quark matter (QM). We found that the shock-induced phase transition (PT) is likely if the density of the star core is more than three times nuclear saturation ([Formula: see text]) density. The conversion process from NS to quark star (QS) is found to be an exothermic process beyond such densities. The burning process at the star center most likely starts as a deflagration process. However, there can be a small window at lower densities where the process can be a detonation one. At small enough infalling matter velocities the resultant magnetic field of the QS is lower than that of the NS. However, for a higher value of infalling matter velocities, the magnetic field of QM becomes larger. Therefore, depending on the initial density fluctuation and on whether the PT is a violent one or not the QS could be more magnetic or less magnetic. The PT also have a considerable effect on the tilt of the magnetic axis of the star. For smaller velocities and densities the magnetic angle are not affected much but for higher infalling velocities tilt of the magnetic axis changes suddenly. The magnetic field strength and the change in the tilt axis can have a significant effect on the observational aspect of the magnetars.

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