scholarly journals The Nuclear Physics of the Neutron Star Crust

2009 ◽  
Author(s):  
Andrew Steiner
Keyword(s):  
Neutron Star ◽  
Nuclear Physics ◽  
Neutron Star Crust

scholarly journals Properties of Neutron Star Crust with Improved Nuclear Physics: Impact of Chiral EFT Interactions and Experimental Nuclear Masses

2021 ◽  
Vol 62 (4) ◽  
Author(s):  
Guilherme Grams ◽  
Jérôme Margueron ◽  
Rahul Somasundaram ◽  
Sanjay Reddy
Keyword(s):  
Neutron Star ◽  
Nuclear Physics ◽  
Neutron Star Crust ◽  
Nuclear Masses

scholarly journals Moment of inertia of neutron star crust in alternative and modified theories of gravity

2016 ◽  
Vol 94 (2) ◽  
Author(s):  
Kalin V. Staykov ◽  
K. Yavuz Ekşi ◽  
Stoytcho S. Yazadjiev ◽  
M. Metehan Türkoğlu ◽  
A. Savaş Arapoğlu
Keyword(s):  
Neutron Star ◽  
Moment Of Inertia ◽  
Modified Theories Of Gravity ◽  
Neutron Star Crust ◽  
Theories Of Gravity

scholarly journals Multimessenger approaches to exploring dense matter in neutron stars

2021 ◽  
Author(s):  
◽  
Lukas Weih
Keyword(s):  
Phase Transition ◽  
Neutron Star ◽  
Nuclear Physics ◽  
Computational Cost ◽  
Dense Matter ◽  
High Energy ◽  
Radiative Transport ◽  
Binary Neutron Star ◽  
Starting Point ◽  
Numerical Astrophysics

High-energy astrophysics plays an increasingly important role in the understanding of our universe. On one hand, this is due to ground-breaking observations, like the gravitational-wave detections of the LIGO and Virgo network or the black-hole shadow observations of the EHT collaboration. On the other hand, the field of numerical relativity has reached a level of sophistication that allows for realistic simulations that include all four fundamental forces of nature. A prime example of how observations and theory complement each other can be seen in the studies following GW170817, the first detection of gravitational waves from a binary neutron-star merger. The same detection is also the chronological starting point of this Thesis. The plethora of information and constraints on nuclear physics derived from GW170817 in conjunction with theoretical computations will be presented in the first part of this Thesis. The second part goes beyond this detection and prepares for future observations when also the high-frequency postmerger signal will become detectable. Specifically, signatures of a quark-hadron phase transition are discussed and the specific case of a delayed phase transition is analyzed in detail. Finally, the third part of this Thesis focuses on the inclusion of radiative transport in numerical astrophysics. In the context of binary neutron-star mergers, radiation in the form of neutrinos is crucial for realistic long-term simulations. Two methods are introduced for treating radiation: the approximate state-of-the-art two-moment method (M1) and the recently developed radiative Lattice-Boltzmann method. The latter promises to be more accurate than M1 at a comparable computational cost. Given that most methods for radiative transport or either inaccurate or unfeasible, the derivation of this new method represents a novel and possibly paradigm-changing contribution to an accurate inclusion of radiation in numerical astrophysics.

scholarly journals Shear viscosity in magnetized neutron star crust

2015 ◽  
Vol 112 (5) ◽  
pp. 59001 ◽  
Author(s):  
D. D. Ofengeim ◽  
D. G. Yakovlev
Keyword(s):  
Neutron Star ◽  
Shear Viscosity ◽  
Neutron Star Crust

scholarly journals Torsional shear oscillations in the neutron star crust driven by the restoring force of elastic stresses

2007 ◽  
Vol 382 (2) ◽  
pp. 849-859 ◽  
Author(s):  
S. I. Bastrukov ◽  
H.- K. Chang ◽  
J. Takata ◽  
G.- T. Chen ◽  
I. V. Molodtsova
Keyword(s):  
Neutron Star ◽  
Restoring Force ◽  
Elastic Stresses ◽  
Neutron Star Crust ◽  
Torsional Shear

scholarly journals Timing of Optical Pulses from the Crab Nebula Pulsar

1971 ◽  
Vol 46 ◽  
pp. 119-124
Author(s):  
P. E. Boynton ◽  
E. J. Groth ◽  
R. B. Partridge ◽  
David T. Wilkinson
Keyword(s):  
Neutron Star ◽  
Crab Nebula ◽  
Physical Models ◽  
Quiet Period ◽  
Eccentric Orbit ◽  
Optical Pulses ◽  
Neutron Star Crust ◽  
Alternate Explanation ◽  
Speed Up ◽  
The Crab Nebula

Timing the arrival of optical pulses from NP 0532 is a potentially important tool for studying the physics of this fascinating object. However, there are some difficulties in interpreting the data in terms of physical models. Some progress has been made on understanding the largest effect – the pulsar braking mechanism. The glitch of late September, 1969 can be interpreted as the speed-up, and subsequent relaxation, of the rotation of a neutron star crust. An alternate explanation is that of a planet in an eccentric orbit. Both models fit the rather meager data near the event. A small sinusoidal effect is indicated in a relatively quiet period of the data.

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