Thermal evolution of neutron stars with decaying magnetic fields

2015 ◽  
Vol 15 (9) ◽  
pp. 1475-1482
Author(s):  
Wei Wei ◽  
Xiao-Ping Zheng ◽  
Xi-Wei Liu
Keyword(s):  
Magnetic Fields ◽  
Neutron Stars ◽  
Thermal Evolution

scholarly journals Evolution of thermally generated neutron-star magnetic Fields

1992 ◽  
Vol 128 ◽  
pp. 46-48
Author(s):  
Roger W. Romani ◽  
Lars E. Hernquist
Keyword(s):  
Neutron Star ◽  
Magnetic Fields ◽  
Neutron Stars ◽  
Magnetic Dipole ◽  
Thermal Evolution ◽  
Magnetic Moments ◽  
New Model ◽  
Wide Range ◽  
Theoretical Evidence ◽  
Hubble Time

AbstractStrongly magnetized neutron stars are believed to underlie a variety of astrophysical systems, although conflicting observational and theoretical evidence has led to debate on the origin and stability of these magnetic fields. Here we describe a new model of neutron star magnetic moments, assuming that the fields are generated at birth and following their evolution to ages as large as the Hubble time. With realistic thermal evolution and conductivities, isolated neutron stars will maintain large magnetic dipole fields. As suggested elsewhere field modification under mass accretion might lead to torque decay. We identify an operative mechanism for this process; the results of this unified picture are in agreement with observations of a wide range of neutron star systems.

scholarly journals Magnetic neutron star cooling and microphysics

2018 ◽  
Vol 609 ◽  
pp. A74 ◽  
Author(s):  
A. Y. Potekhin ◽  
G. Chabrier
Keyword(s):  
Neutron Star ◽  
Finite Difference ◽  
Magnetic Fields ◽  
Neutron Stars ◽  
Thermodynamic Functions ◽  
Thermal Evolution ◽  
Relative Importance ◽  
Quasistationary Approximation ◽  
Theoretical Predictions ◽  
Neutron Star Cooling

Aims. We study the relative importance of several recent updates of microphysics input to the neutron star cooling theory and the effects brought about by superstrong magnetic fields of magnetars, including the effects of the Landau quantization in their crusts. Methods. We use a finite-difference code for simulation of neutron-star thermal evolution on timescales from hours to megayears with an updated microphysics input. The consideration of short timescales (≲1 yr) is made possible by a treatment of the heat-blanketing envelope without the quasistationary approximation inherent to its treatment in traditional neutron-star cooling codes. For the strongly magnetized neutron stars, we take into account the effects of Landau quantization on thermodynamic functions and thermal conductivities. We simulate cooling of ordinary neutron stars and magnetars with non-accreted and accreted crusts and compare the results with observations. Results. Suppression of radiative and conductive opacities in strongly quantizing magnetic fields and formation of a condensed radiating surface substantially enhance the photon luminosity at early ages, making the life of magnetars brighter but shorter. These effects together with the effect of strong proton superfluidity, which slows down the cooling of kiloyear-aged neutron stars, can explain thermal luminosities of about a half of magnetars without invoking heating mechanisms. Observed thermal luminosities of other magnetars are still higher than theoretical predictions, which implies heating, but the effects of quantizing magnetic fields and baryon superfluidity help to reduce the discrepancy.

Joule Heating and the Thermal Evolution of Old Neutron Stars

1998 ◽  
Vol 503 (1) ◽  
pp. 368-373 ◽  
Author(s):  
Juan A. Miralles ◽  
Vadim Urpin ◽  
Denis Konenkov
Keyword(s):  
Neutron Stars ◽  
Joule Heating ◽  
Thermal Evolution

scholarly journals Planetary Magnetic Fields and Habitability in Super Earths

2018 ◽  
Vol 27 (1) ◽  
pp. 183-231 ◽  
Author(s):  
Pablo Cuartas-Restrepo
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Scaling Laws ◽  
Thermal Evolution ◽  
Solid Core ◽  
Direct Influence ◽  
Physical Processes ◽  
Planetary Magnetic Fields ◽  
Planetary Magnetic Field ◽  
Planetary Dynamos

Abstract This work seeks to summarize some special aspects of a type of exoplanets known as super-Earths (SE), and the direct influence of these aspects in their habitability. Physical processes like the internal thermal evolution and the generation of a protective Planetary Magnetic Field (PMF) are directly related with habitability. Other aspects such as rotation and the formation of a solid core are fundamental when analyzing the possibilities that a SE would have to be habitable. This work analyzes the fundamental theoretical aspects on which the models of thermal evolution and the scaling laws of the planetary dynamos are based. These theoretical aspects allow to develop models of the magnetic evolution of the planets and the role played by the PMF in the protection of the atmosphere and the habitability of the planet.

Origin of Magnetic Fields in White Dwarfs and Neutron Stars

1971 ◽  
Vol 231 (19) ◽  
pp. 32-33 ◽  
Author(s):  
R. F. O'CONNELL ◽  
K. M. ROUSSEL
Keyword(s):  
Magnetic Fields ◽  
Neutron Stars ◽  
White Dwarfs

Effect of Superstrong Magnetic Fields on Nuclear Energy Generation Rate in the Crust of Neutron Stars

2008 ◽  
Vol 49 (4) ◽  
pp. 1069-1072 ◽  
Author(s):  
Liu Hong-Lin ◽  
Luo Zhi-Quan ◽  
Liu Jing-Jing ◽  
Lai Xiang-Jun
Keyword(s):  
Magnetic Fields ◽  
Neutron Stars ◽  
Nuclear Energy ◽  
Energy Generation ◽  
Generation Rate

scholarly journals Nuclear equation of state and neutron star cooling

2017 ◽  
Vol 26 (04) ◽  
pp. 1750015 ◽  
Author(s):  
Yeunhwan Lim ◽  
Chang Ho Hyun ◽  
Chang-Hwan Lee
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Thermal Evolution ◽  
Observation Data ◽  
Nuclear Equation Of State ◽  
The Core ◽  
Dense Nuclear Matter ◽  
Nuclear Models

In this paper, we investigate the cooling of neutron stars with relativistic and nonrelativistic models of dense nuclear matter. We focus on the effects of uncertainties originated from the nuclear models, the composition of elements in the envelope region, and the formation of superfluidity in the core and the crust of neutron stars. Discovery of [Formula: see text] neutron stars PSR J1614−2230 and PSR J0343[Formula: see text]0432 has triggered the revival of stiff nuclear equation of state at high densities. In the meantime, observation of a neutron star in Cassiopeia A for more than 10 years has provided us with very accurate data for the thermal evolution of neutron stars. Both mass and temperature of neutron stars depend critically on the equation of state of nuclear matter, so we first search for nuclear models that satisfy the constraints from mass and temperature simultaneously within a reasonable range. With selected models, we explore the effects of element composition in the envelope region, and the existence of superfluidity in the core and the crust of neutron stars. Due to uncertainty in the composition of particles in the envelope region, we obtain a range of cooling curves that can cover substantial region of observation data.

Physics in Strong Magnetic Fields Near Neutron Stars

Science ◽  
1991 ◽  
Vol 251 (4997) ◽  
pp. 1033-1038 ◽  
Author(s):  
A. K. HARDING
Keyword(s):  
Magnetic Fields ◽  
Neutron Stars ◽  
Strong Magnetic Fields

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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