Gravitational wave afterglow in binary neutron star mergers

Doneva, Daniela D.; Kokkotas, Kostas D.; Pnigouras, Pantelis

doi:10.1103/physrevd.92.104040

Cited by 83 publications

(131 citation statements)

References 46 publications

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“…Our observational constraints would also be weakened if a large fraction of the magnetar rotational energy is emitted as gravitational waves instead of through electromagnetic spindown (e.g., Doneva et al 2015;Gao et al 2016;Lasky & Glampedakis 2016). This could occur either due to a misalignment between the rotation axis and the magnetic dipole axis (e.g., Dall'Osso et al 2009) or via the growth of the f-mode instability (e.g., Doneva et al 2015).…”

Section: Discussionmentioning

confidence: 94%

Radio Constraints on Long-Lived Magnetar Remnants in Short Gamma-Ray Bursts

Fong

Metzger

Berger

et al. 2016

ApJ

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The merger of a neutron star (NS) binary may result in the formation of a rapidly spinning magnetar. The magnetar can potentially survive for seconds or longer as a supramassive NS before collapsing to a black hole if, indeed, it collapses at all. During this process, a fraction of the magnetar's rotational energy of ∼10 53 erg is transferred via magnetic spin-down to the surrounding ejecta. The resulting interaction between the ejecta and the surrounding circumburst medium powers a year-long or greater synchrotron radio transient. We present a search for radio emission with the Very Large Array following nine short-duration gamma-ray bursts (GRBs) at rest-frame times of ≈1.3-7.6 yr after the bursts, focusing on those events that exhibit early-time excess X-ray emission that may signify the presence of magnetars. We place upper limits of 18-32 μJy on the 6.0 GHz radio emission, corresponding to spectral luminosities of (0.05-8.3)×10 39 erg s −1 . Comparing these limits to the predicted radio emission from a long-lived remnant and incorporating measurements of the circumburst densities from broadband modeling of short GRB afterglows, we rule out a stable magnetar with an energy of 10 53 erg for half of the events in our sample. A supramassive remnant that injects a lower rotational energy of 10 52 erg is ruled out for a single event, GRB 050724A. This study represents the deepest and most extensive search for long-term radio emission following short GRBs to date, and thus the most stringent limits placed on the physical properties of magnetars associated with short GRBs from radio observations.

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Section: Discussionmentioning

confidence: 94%

Radio Constraints on Long-Lived Magnetar Remnants in Short Gamma-Ray Bursts

Fong

Metzger

Berger

et al. 2016

ApJ

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“…Clark et al 2014) can produce a measurable GW signal for hundreds of milliseconds following the merger and provide information on the NS EOS, but they are unlikely to provide unambiguous evidence for an extremely long remnant lifetime (the ringdown signature of the newly-formed BH will probably not be measurable). The magnetar itself will produce a periodic gravitational wave signal; however, its strength depends on the presence of a strong toroidal magnetic field misaligned with the rotation axis (e.g., Stella et al 2005;Fan et al 2013;Lasky et al 2014;Dall'Osso et al 2015) or the growth and saturation of the f-mode instability (e.g., Doneva et al 2015).…”

Section: Discussionmentioning

confidence: 99%

High-energy Neutrinos from Millisecond Magnetars Formed from the Merger of Binary Neutron Stars

Fang¹,

Metzger²

2017

ApJ

113

129

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The merger of a neutron star (NS) binary may result in the formation of a long-lived, or indefinitely stable, millisecond magnetar remnant surrounded by a low-mass ejecta shell. A portion of the magnetar's prodigious rotational energy is deposited behind the ejecta in a pulsar wind nebula, powering luminous optical/X-ray emission for hours to days following the merger. Ions in the pulsar wind may also be accelerated to ultra-high energies, providing a coincident source of high energy cosmic rays and neutrinos. At early times, the cosmic rays experience strong synchrotron losses; however, after a day or so, pion production through photomeson interaction with thermal photons in the nebula comes to dominate, leading to efficient production of high-energy neutrinos. After roughly a week, the density of background photons decreases sufficiently for cosmic rays to escape the source without secondary production. These competing effects result in a neutrino light curve that peaks on a few day timescale near an energy of ∼ 10 18 eV. This signal may be detectable for individual mergers out to ∼ 10 (100) Mpc by current (next-generation) neutrino telescopes, providing clear evidence for a long-lived NS remnant, the presence of which may otherwise be challenging to identify from the gravitational waves alone. Under the optimistic assumption that a sizable fraction of NS mergers produce long-lived magnetars, the cumulative cosmological neutrino background is estimated to be ∼ 10 −9 − 10 −8 GeV cm −2 s −1 sr −1 for a NS merger rate of 10 −7 Mpc −3 yr −1 , overlapping with IceCube's current sensitivity and within the reach of next-generation neutrino telescopes.

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“…Four different parameterized fits to the expected evolution of the CSFR density have been extracted from Hopkins & Beacom (2006), Fardal et al (2007), Wilkins et al (2008), Robertson & Ellis (2012) in order to account for the uncertainty upon its determination. The f -mode frequencies and the instability windows have been extracted from Doneva et al (2013Doneva et al ( , 2015 for supernova and merger derived NSs respectively, for a relativistic star with the WFF2 EoS in the Cowling approximation.…”

Section: Discussionmentioning

confidence: 99%

“…For NSs formed from binary mergers, all of the stars are expected to initially rotate at the Kepler limit. We also assume that both NS classes rotate uniformly, since differential rotation is expected to disappear shortly after the star's formation (Doneva et al 2015, and references therein).…”

Section: The Evolution Of the F -Mode Instabilitymentioning

confidence: 99%

The stochastic background of gravitational waves due to thef-mode instability in neutron stars

Surace¹,

Kokkotas²,

Pnigouras³

2016

A&A

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This paper presents an estimate for the spectral properties of the stochastic background of gravitational waves emitted by a population of hot, young, rapidly rotating neutron stars throughout the Universe undergoing f -mode instabilities, formed through either corecollapse supernova explosions or the merger of binary neutron star systems. Their formation rate, from which the gravitational wave event rate is obtained, is deduced from observation-based determinations of the cosmic star formation rate. The gravitational wave emission occurs during the spin-down phase of the f -mode instability. For low magnetized neutron stars and assuming 10% of supernova events lead to f -mode unstable neutron stars, the background from supernova-derived neutron stars peaks at Ω gw ∼ 10 −9 for the l = m = 2 f -mode, which should be detectable by cross-correlating a pair of second generation interferometers (e.g. Advanced LIGO/Virgo) with an upper estimate for the signal-to-noise ratio of ≈9.8. The background from supramassive neutron stars formed from binary mergers peaks at Ω gw ∼ 10 −10 and should not be detectable, even with third generation interferometers (e.g. Einstein Telescope).

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Gravitational wave afterglow in binary neutron star mergers

Cited by 83 publications

References 46 publications

Radio Constraints on Long-Lived Magnetar Remnants in Short Gamma-Ray Bursts

Radio Constraints on Long-Lived Magnetar Remnants in Short Gamma-Ray Bursts

High-energy Neutrinos from Millisecond Magnetars Formed from the Merger of Binary Neutron Stars

The stochastic background of gravitational waves due to thef-mode instability in neutron stars

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