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Dive into the research topics where Curran D. Muhlberger is active.

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Featured researches published by Curran D. Muhlberger.


The Astrophysical Journal | 2013

BLACK HOLE-NEUTRON STAR MERGERS WITH A HOT NUCLEAR EQUATION OF STATE: OUTFLOW AND NEUTRINO-COOLED DISK FOR A LOW-MASS, HIGH-SPIN CASE

M. Brett Deaton; Matthew D. Duez; Francois Foucart; Evan O'Connor; Christian D. Ott; Lawrence E. Kidder; Curran D. Muhlberger; Mark A. Scheel; Bela Szilagyi

Neutrino emission significantly affects the evolution of the accretion tori formed in black hole-neutron star mergers. It removes energy from the disk, alters its composition, and provides a potential power source for a gamma-ray burst. To study these effects, simulations in general relativity with a hot microphysical equation of state (EOS) and neutrino feedback are needed. We present the first such simulation, using a neutrino leakage scheme for cooling to capture the most essential effects and considering a moderate mass (1.4 M_☉ neutron star, 5.6 M_☉ black hole), high-spin (black hole J/M^2 = 0.9) system with the K_0 = 220 MeV Lattimer-Swesty EOS. We find that about 0.08 M_☉ of nuclear matter is ejected from the system, while another 0.3 M_☉ forms a hot, compact accretion disk. The primary effects of the escaping neutrinos are (1) to make the disk much denser and more compact, (2) to cause the average electron fraction Ye of the disk to rise to about 0.2 and then gradually decrease again, and (3) to gradually cool the disk. The disk is initially hot (T ~ 6 MeV) and luminous in neutrinos (L_ν ~ 10^54 erg s^–1), but the neutrino luminosity decreases by an order of magnitude over 50 ms of post-merger evolution.


Physical Review D | 2016

Simulations of inspiraling and merging double neutron stars using the Spectral Einstein Code

Roland Haas; Christian D. Ott; Bela Szilagyi; Jeffrey D. Kaplan; Jonas Lippuner; Mark A. Scheel; K. Barkett; Curran D. Muhlberger; Tim Dietrich; Matthew D. Duez; Francois Foucart; Harald P. Pfeiffer; Lawrence E. Kidder; Saul A. Teukolsky

We present results on the inspiral, merger, and postmerger evolution of a neutron star-neutron star (NSNS) system. Our results are obtained using the hybrid pseudospectral-finite volume Spectral Einstein Code (SpEC). To test our numerical methods, we evolve an equal-mass system for ≈22 orbits before merger. This waveform is the longest waveform obtained from fully general-relativistic simulations for NSNSs to date. Such long (and accurate) numerical waveforms are required to further improve semianalytical models used in gravitational wave data analysis, for example, the effective one body models. We discuss in detail the improvements to SpEC’s ability to simulate NSNS mergers, in particular mesh refined grids to better resolve the merger and postmerger phases. We provide a set of consistency checks and compare our results to NSNS merger simulations with the independent bam code. We find agreement between them, which increases confidence in results obtained with either code. This work paves the way for future studies using long waveforms and more complex microphysical descriptions of neutron star matter in SpEC.


Physical Review D | 2016

Gravitational waveforms for neutron star binaries from binary black hole simulations

K. Barkett; Mark A. Scheel; Roland Haas; Christian D. Ott; Sebastiano Bernuzzi; D. A. Brown; Bela Szilagyi; Jeffrey D. Kaplan; Jonas Lippuner; Curran D. Muhlberger; Francois Foucart; Matthew D. Duez

Gravitational waves from binary neutron star (BNS) and black-hole/neutron star (BHNS) inspirals are primary sources for detection by the Advanced Laser Interferometer Gravitational-Wave Observatory. The tidal forces acting on the neutron stars induce changes in the phase evolution of the gravitational waveform, and these changes can be used to constrain the nuclear equation of state. Current methods of generating BNS and BHNS waveforms rely on either computationally challenging full 3D hydrodynamical simulations or approximate analytic solutions. We introduce a new method for computing inspiral waveforms for BNS/BHNS systems by adding the post-Newtonian (PN) tidal effects to full numerical simulations of binary black holes (BBHs), effectively replacing the non-tidal terms in the PN expansion with BBH results. Comparing a waveform generated with this method against a full hydrodynamical simulation of a BNS inspiral yields a phase difference of < 1 radian over ~ 15 orbits. The numerical phase accuracy required of BNS simulations to measure the accuracy of the method we present here is estimated as a function of the tidal deformability parameter ⋋.


Physical Review D | 2015

Binary Neutron Stars with Arbitrary Spins in Numerical Relativity

Nick Tacik; Francois Foucart; Harald P. Pfeiffer; Roland Haas; S. Ossokine; Jeff Kaplan; Curran D. Muhlberger; Matt D. Duez; Lawrence E. Kidder; Mark A. Scheel; Bela Szilagyi

We present a code to construct initial data for binary neutron star systems in which the stars are rotating. Our code, based on a formalism developed by Tichy, allows for arbitrary rotation axes of the neutron stars and is able to achieve rotation rates near rotational breakup. We compute the neutron star angular momentum through quasilocal angular momentum integrals. When constructing irrotational binary neutron stars, we find a very small residual dimensionless spin of ∼2×10^(−4). Evolutions of rotating neutron star binaries show that the magnitude of the stars’ angular momentum is conserved, and that the spin and orbit precession of the stars is well described by post-Newtonian approximation. We demonstrate that orbital eccentricity of the binary neutron stars can be controlled to ∼0.1%. The neutron stars show quasinormal mode oscillations at an amplitude which increases with the rotation rate of the stars.


The Astrophysical Journal | 2016

ERRATUM: “BLACK HOLE–NEUTRON STAR MERGERS WITH A HOT NUCLEAR EQUATION OF STATE: OUTFLOW AND NEUTRINO-COOLED DISK FOR A LOW-MASS, HIGH-SPIN CASE” (2013, ApJ, 776, 47)

M. Brett Deaton; Matthew D. Duez; Francois Foucart; Evan O’Connor; Christian D. Ott; Lawrence E. Kidder; Curran D. Muhlberger; Mark A. Scheel; Bela Szilagyi

M. Brett Deaton, Matthew D. Duez, Francois Foucart, Evan O’Connor, Christian D. Ott, Lawrence E. Kidder, Curran D. Muhlberger, Mark A. Scheel, and Bela Szilagyi 1 Department of Physics & Astronomy, Washington State University, Pullman, Washington 99164, USA; [email protected], [email protected] 2 Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario M5S 3H8, Canada 3 TAPIR, MC 350-17, California Institute of Technology, Pasadena, California 91125, USA 4 Center for Radiophysics and Space Research, Cornell University, Ithaca, New York, 14853, USA Received 2016 April 21; accepted 2016 May 2; published 2016 June 13


Classical and Quantum Gravity | 2016

Initial data for black hole–neutron star binaries, with rotating stars

Nick Tacik; Francois Foucart; Harald P. Pfeiffer; Curran D. Muhlberger; Lawrence E. Kidder; Mark A. Scheel; Bela Szilagyi

The coalescence of a neutron star with a black hole is a primary science target of ground-based gravitational wave detectors. Constraining or measuring the neutron star spin directly from gravitational wave observations requires knowledge of the dependence of the emission properties of these systems on the neutron star spin. This paper lays foundations for this task, by developing a numerical method to construct initial data for black hole–neutron star binaries with arbitrary spin on the neutron star. We demonstrate the robustness of the code by constructing initial-data sets in large regions of the parameter space. In addition to varying the neutron star spin-magnitude and spin-direction, we also explore neutron star compactness, mass-ratio, black hole spin, and black hole spin-direction. Specifically, we are able to construct initial data sets with neutron stars spinning near centrifugal break-up, and with black hole spins as large as S_(BH) / M_(BH)^2 = 0.99.


Physical Review D | 2014

Magnetic effects on the low-T/|W| instability in differentially rotating neutron stars

Curran D. Muhlberger; Fatemeh Hossein Nouri; Matthew D. Duez; Francois Foucart; Lawrence E. Kidder; Christian D. Ott; Mark A. Scheel; Bela Szilagyi; Saul A. Teukolsky


Archive | 2010

Simulations of Neutron-Star Binaries using the Spectral Einstein Code (SpEC)

Jeffrey D. Kaplan; Christian D. Ott; Curran D. Muhlberger; Matthew D. Duez; Francois Foucart; Mark A. Scheel


Physical Review D | 2016

Erratum: Binary neutron stars with arbitrary spins in numerical relativity [Phys. Rev. D92, 124012 (2015)]

Nick Tacik; Francois Foucart; Harald P. Pfeiffer; Roland Haas; Serguei Ossokine; Jeff Kaplan; Curran D. Muhlberger; Matt D. Duez; Lawrence E. Kidder; Mark A. Scheel; Bela Szilagyi


Archive | 2014

Magnetic e ects on the low-T=jWj instability in di erentially rotating neutron stars

Curran D. Muhlberger; Fatemeh Hossein Nouri; Matthew D. Duez; Francois Foucart; Lawrence E. Kidder; Christian D. Ott; Mark A. Scheel; Saul A. Teukolsky

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Mark A. Scheel

California Institute of Technology

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Matthew D. Duez

Washington State University

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Christian D. Ott

California Institute of Technology

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Jeffrey D. Kaplan

California Institute of Technology

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