Dome Design Brings Numerical Astrophysics Down to Earth

1997 ◽  
Vol 11 (3) ◽  
pp. 220
Author(s):  
Patricia Daukantas
Keyword(s):  
Numerical Astrophysics

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.

Numerical Astrophysics

2007 ◽  
Vol 328 (7) ◽  
pp. 661-664
Author(s):  
Christian Klingenberg
Keyword(s):  
Numerical Astrophysics

scholarly journals Visualization Methods for Numerical Astrophysics

Astrophysics ◽  
10.5772/32203 ◽  
2012 ◽  
Author(s):  
Werner Benger ◽  
Markus Haider ◽  
Josef Stoeckl ◽  
Biagio Cosenza ◽  
Marcel Ritter ◽  
...  
Keyword(s):  
Numerical Astrophysics

scholarly journals ISENTROPIC "SHOCK WAVES" IN NUMERICAL ASTROPHYSICS

2016 ◽  
Vol 29 (0) ◽  
pp. 54-57
Author(s):  
S. G. Moiseenko ◽  
G. S. Bisnovatyi-Kogan
Keyword(s):  
Shock Waves ◽  
Numerical Astrophysics

scholarly journals Supernova-driven interstellar turbulence and the galactic dynamo

2010 ◽  
Vol 6 (S274) ◽  
pp. 348-354
Author(s):  
Oliver Gressel ◽  
Detlef Elstner ◽  
Günther Rüdiger
Keyword(s):  
Mean Field ◽  
Field Method ◽  
Test Field ◽  
Dynamo Theory ◽  
Quasilinear Theory ◽  
Interstellar Turbulence ◽  
Supernova Explosions ◽  
The Mean ◽  
Numerical Astrophysics

AbstractThe fractal shape and multi-component nature of the interstellar medium together with its vast range of dynamical scales provides one of the great challenges in theoretical and numerical astrophysics. Here we will review recent progress in the direct modelling of interstellar hydromagnetic turbulence, focusing on the role of energy injection by supernova explosions. The implications for dynamo theory will be discussed in the context of the mean-field approach.Results obtained with the test field-method are confronted with analytical predictions and estimates from quasilinear theory. The simulation results enforce the classical understanding of a turbulent Galactic dynamo and, more importantly, yield new quantitative insights. The derived scaling relations enable confident global mean-field modelling.

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