Matthew Anderson

Magnetized Neutron-Star Mergers and Gravitational-Wave Signals

We investigate the influence of magnetic fields upon the dynamics of, and resulting gravitational waves from, a binary neutron-star merger in full general relativity coupled to ideal magnetohydrodynamics. We consider two merger scenarios: one where the stars have aligned poloidal magnetic fields and one without. Both mergers result in a strongly differentially rotating object. In comparison to the nonmagnetized scenario, the aligned magnetic fields delay the full merger of the stars. During and after merger we observe phenomena driven by the magnetic field, including Kelvin-Helmholtz instabilities in shear layers, winding of the field lines, and transition from poloidal to toroidal magnetic fields. These effects not only mediate the production of electromagnetic radiation, but also can have a strong influence on the gravitational waves. Thus, there are promising prospects for studying such systems with both types of waves.

Effects of the microphysical Equation of State in the mergers of magnetized Neutron Stars With Neutrino Cooling

We study the merger of binary neutron stars using different realistic, microphysical nuclear equations of state, as well as incorporating magnetic field and neutrino cooling effects. In particular, we concentrate on the influence of the equation of state on the gravitational wave signature and also on its role, in combination with cooling and electromagnetic effects, in determining the properties of the hypermassive neutron star resulting from the merger, the production of neutrinos, and the characteristics of ejecta from the system. The ejecta we find are consistent with other recent studies that find soft equations of state produce more ejecta than stiffer equations of state. Moreover, the degree of neutron richness increases for softer equations of state. In light of reported kilonova observations (associated to GRB~130603B and GRB~060614) and the discovery of relatively low abundances of heavy, radioactive elements in deep sea deposits (with respect to possible production via supernovae), we speculate that a soft EoS might be preferred---because of its significant production of sufficiently neutron rich ejecta---if such events are driven by binary neutron star mergers. We also find that realistic magnetic field strengths, obtained with a sub-grid model tuned to capture magnetic amplification via the Kelvin-Helmholtz instability at merger, are generally too weak to affect the gravitational wave signature post-merger within a time scale of

Electromagnetic and gravitational outputs from binary-neutron-star coalescence.

\approx 10

Preliminary design examination of the ParalleX system from a software and hardware perspective

~ms but can have subtle effects on the post-merger dynamics.

Improving the scalability of parallel N-body applications with an event-driven constraint-based execution model

Carlos Palenzuela, Luis Lehner, Marcelo Ponce, Steven L. Liebling, Matthew Anderson, David Neilsen, and Patrick Motl Canadian Institute for Theoretical Astrophysics, Toronto, Ontario M5S 3H8, Canada, Perimeter Institute for Theoretical Physics,Waterloo, Ontario N2L 2Y5, Canada Department of Physics, University of Guelph, Guelph, Ontario N1G 2W1, Canada, Department of Physics, Long Island University, New York 11548, USA 5 Pervasive Technology Institute, Indiana University, Bloomington, IN 47405, USA Department of Physics and Astronomy, Brigham Young University, Provo, Utah 84602, USA, Department of Science, Mathematics and Informatics, Indiana University Kokomo, Kokomo, IN 46904, USA,

Magnetized Neutron Stars With Realistic Equations of State and Neutrino Cooling

Exascale systems, expected to emerge by the end of the next decade, will require the exploitation of billion-way parallelism at multiple hierarchical levels in order to achieve the desired sustained performance. While traditional approaches to performance evaluation involve measurements of existing applications on the available platforms, such a methodology is obviously unsuitable for architectures still at the brainstorming stage. The prediction of the future machine performance is an important factor driving the design of both the execution hardware and software environment. A good way to start assessing the performance is to identify the factors challenging the scalability of parallel applications. We believe the root cause of these challenges is the incoherent coupling between the current enabling technologies, such as Non-Uniform Memory Access of present multicore nodes equipped with optional hardware accelerators and the decades older execution model, i.e., Communicating Sequential Processes (CSP). Supercomputing is in the midst of a much needed phase change and the High-Performance Computing community is slowly realizing the necessity for a new design dogma, as affirmed in the preliminary Exascale studies. In this paper, we present an overview of the ParalleX execution model and its complementary design efforts at the software and hardware levels, while including power draw of the system as the resource of utmost importance. Since the interplay of hardware and software environment is quickly becoming one of the dominant factors in the design of well integrated, energy efficient, large-scale systems, we also explore the implications of the ParalleX model on the organization of parallel computing architectures. We also present scaling and performance results for an adaptive mesh refinement application developed using a ParalleX-compliant runtime system implementation, HPX.

Unequal mass binary neutron star mergers and multimessenger signals

The scalability and efficiency of graph applications are significantly constrained by conventional systems and their supporting programming models. Technology trends such as multicore, manycore, and heterogeneous system architectures are introducing further challenges and possibilities for emerging application domains such as graph applications. This paper explores the parallel execution of graphs that are generated using the Barnes–Hut algorithm to exemplify dynamic workloads. The workloads are expressed using the semantics of an exascale computing execution model called ParalleX. For comparison, results using conventional execution model semantics are also presented. We find improved load balancing during runtime and automatic parallelism discovery by using the advanced semantics for exascale computing.

Linking electromagnetic and gravitational radiation in coalescing binary neutron stars

We incorporate realistic, tabulated equations of state into fully relativistic simulations of magnetized neutron stars along with a neutrino leakage scheme which accounts for cooling via neutrino emission. Both these improvements utilize open-source code (GR1D) and tables from this http URL Our implementation makes use of a novel method for the calculation of the optical depth which simplifies its use with distributed adaptive mesh refinement. We present various tests with and without magnetization and preliminary results both from single stars and from the merger of a binary system.

A Dynamic Execution Model Applied to Distributed Collision Detection

We study the merger of binary neutron stars with different mass ratios adopting three different realistic, microphysical nuclear equations of state, as well as incorporating neutrino cooling effects. In particular, we concentrate on the influence of the equation of state on the gravitational wave signature and also on its role, in combination with neutrino cooling, in determining the properties of the resulting hypermassive neutron star, of the neutrinos produced, and of the ejected material. The ejecta we find are consistent with other recent studies that find that small mass ratios produce more ejecta than equal mass cases (up to some limit) and this ejecta is more neutron rich. This trend indicates the importance with future kilonovae observations of measuring the individual masses of an associated binary neutron star system, presumably from concurrent gravitational wave observations, in order to be able to extract information about the nuclear equation of state

Towards Exascale Co-design in a Runtime System

We expand on our study of the gravitational and electromagnetic emissions from the late stage of an inspiraling neutron star binary as presented in Palenzuela et al. [Phys. Rev. Lett. 111, 061105 (2013)]. Interactions between the stellar magnetospheres, driven by the extreme dynamics of the merger, can yield considerable outflows. We study the gravitational and electromagnetic waves produced during the inspiral and merger of a binary neutron star system using a full relativistic, resistive magnetohydrodynamics evolution code. We show that the interaction between the stellar magnetospheres extracts kinetic energy from the system and powers radiative Poynting flux and heat dissipation. These features depend strongly on the configuration of the initial stellar magnetic moments. Our results indicate that this power can strongly outshine pulsars in binaries and have a distinctive angular and time-dependent pattern. Our discussion provides more detail than Palenzuela et al., showing clear evidence of the different effects taking place during the inspiral. Our simulations include a few milliseconds after the actual merger and study the dynamics of the magnetic fields during the formation of the hypermassive neutron star. We also briefly discuss the possibility of observing such emissions.