English
 
User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
  Numerical simulations of neutron star-black hole binaries in the near-equal-mass regime

Foucart, F., Duez, M. D., Kidder, L. E., Nissanke, S., Pfeiffer, H. P., & Scheel, M. A. (2019). Numerical simulations of neutron star-black hole binaries in the near-equal-mass regime. Physical Review D, 99(10): 103025. doi:10.1103/PhysRevD.99.103025.

Item is

Basic

show hide
Item Permalink: http://hdl.handle.net/21.11116/0000-0003-652E-9 Version Permalink: http://hdl.handle.net/21.11116/0000-0003-BFFF-8
Genre: Journal Article

Files

show Files
hide Files
:
1903.09166.pdf (Preprint), 621KB
Name:
1903.09166.pdf
Description:
File downloaded from arXiv at 2019-04-15 09:21
Visibility:
Public
MIME-Type / Checksum:
application/pdf / [MD5]
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
:
PhysRevD.99.103025.pdf (Publisher version), 2MB
 
File Permalink:
-
Name:
PhysRevD.99.103025.pdf
Description:
-
Visibility:
Restricted (Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Potsdam-Golm; )
MIME-Type / Checksum:
application/pdf
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
License:
-

Locators

show

Creators

show
hide
 Creators:
Foucart, F., Author
Duez, M. D., Author
Kidder, L. E., Author
Nissanke, S., Author
Pfeiffer, Harald P.1, Author              
Scheel, M. A., Author
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              

Content

show
hide
Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,General Relativity and Quantum Cosmology, gr-qc
 Abstract: Simulations of neutron star-black hole (NSBH) binaries generally consider black holes with masses in the range $(5-10)M_\odot$, where we expect to find most stellar mass black holes. The existence of lower mass black holes, however, cannot be theoretically ruled out. Low-mass black holes in binary systems with a neutron star companion could mimic neutron star-neutron (NSNS) binaries, as they power similar gravitational wave (GW) and electromagnetic (EM) signals. To understand the differences and similarities between NSNS mergers and low-mass NSBH mergers, numerical simulations are required. Here, we perform a set of simulations of low-mass NSBH mergers, including systems compatible with GW170817. Our simulations use a composition and temperature dependent equation of state (DD2) and approximate neutrino transport, but no magnetic fields. We find that low-mass NSBH mergers produce remnant disks significantly less massive than previously expected, and consistent with the post-merger outflow mass inferred from GW170817 for moderately asymmetric mass ratio. The dynamical ejecta produced by systems compatible with GW170817 is negligible except if the mass ratio and black hole spin are at the edge of the allowed parameter space. That dynamical ejecta is cold, neutron-rich, and surprisingly slow for ejecta produced during the tidal disruption of a neutron star : $v\sim (0.1-0.15)c$. We also find that the final mass of the remnant black hole is consistent with existing analytical predictions, while the final spin of that black hole is noticeably larger than expected -- up to $\chi_{\rm BH}=0.84$ for our equal mass case.

Details

show
hide
Language(s):
 Dates: 2019-03-212019
 Publication Status: Published in print
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1903.09166
URI: http://arxiv.org/abs/1903.09166
DOI: 10.1103/PhysRevD.99.103025
 Degree: -

Event

show

Legal Case

show

Project information

show

Source 1

show
hide
Title: Physical Review D
Source Genre: Journal
 Creator(s):
Affiliations:
Publ. Info: -
Pages: - Volume / Issue: 99 (10) Sequence Number: 103025 Start / End Page: - Identifier: -