Abstract
The next generation gravitational waves (GW) detectors are most sensitive to GW emitted by compact (neutron star/black hole) binary mergers. If one of those is a neutron star the merger will also emit electromagnetic radiation via three possible channels: gamma-ray bursts and their (possibly orphan) afterglows, Li-Paczynski Macronovae and radio flares. This accompanying electromagnetic radiation is vitally important in confirming the GW detections. It could also reveal a wealth of information regarding the merger and will open a window towards multimessenger astronomy. Identifying and characterizing these counterparts is therefore of utmost importance. In this work, we explore late time radio flares emitted by the dynamically ejected outflows. We build upon previous work and consider the effect of the outflow's nontrivial geometry. Using an approximate method, we estimate the radio light-curves for several ejected matter distributions obtained in numerical simulations. Our method provides an upper limit to the effect of non-sphericity. Together with the spherical estimates, the resulting light curves bound the actual signal. We find that while non-spherical geometries can in principle lead to an enhanced emission, in most cases they result in an increase in the time-scale compared with a corresponding spherical configuration. This would weaken somewhat these signals and might decrease the detection prospects.
Original language | English |
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Pages (from-to) | 3419-3434 |
Number of pages | 16 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 452 |
Issue number | 4 |
DOIs | |
State | Published - 16 Jul 2015 |
Externally published | Yes |
Bibliographical note
Publisher Copyright:© 2015 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.
Keywords
- Binaries: general
- Gamma-ray burst: general
- Gravitational waves
- Hydrodynamics
- Radio continuum: general
- Stars: neutron