General relativistic magnetohydrodynamic simulations of binary neutron star mergers with the APR4 equation of state

Endrizzi, Andrea; Ciolfi, R.; Giacomazzo, B.; Kastaun, W.; Kawamura, Takumu

doi:10.1088/0264-9381/33/16/164001

Cited by 100 publications

(129 citation statements)

References 54 publications

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“…For example, short-lived hypermassive NSs are expected to emit a few percent of a solar mass in GW energy (e.g., see the two lower dashed lines in Figure 1 that represent 1% and 10% of a solar mass; Kiuchi et al 2009;Clark et al 2014;Bernuzzi et al 2015b;Endrizzi et al 2016;Dietrich et al 2017aDietrich et al , 2017bFeo et al 2017), while our minimum 50% efficiency is   E M c 4.8 Corsi & Mészáros 2009). Figure 1 shows the h rss 50% for the considered waveform models as a function of the waveform's signal-weighted frequency.…”

Section: Implications and Conclusionmentioning

confidence: 99%

Search for Post-merger Gravitational Waves from the Remnant of the Binary Neutron Star Merger GW170817

Abbott¹,

Abbott²,

Abbott³

et al. 2017

ApJL

238

188

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The first observation of a binary neutron star (NS) coalescence by the Advanced LIGO and Advanced Virgo gravitational-wave (GW) detectors offers an unprecedented opportunity to study matter under the most extreme conditions. After such a merger, a compact remnant is left over whose nature depends primarily on the masses of the inspiraling objects and on the equation of state of nuclear matter. This could be either a black hole (BH) or an NS, with the latter being either long-lived or too massive for stability implying delayed collapse to a BH. Here, we present a search for GWs from the remnant of the binary NS merger GW170817 using data from Advanced LIGO and Advanced Virgo. We search for short-(1 s) and intermediate-duration (500 s) signals, which include GW emission from a hypermassive NS or supramassive NS, respectively. We find no signal from the post-merger remnant. Our derived strain upper limits are more than an order of magnitude larger than those predicted by most models. For short signals, our best upper limit on the root sum square of the GW strain emitted from 1-4 kHz is =´--h 2.1 10 Hz

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Section: Implications and Conclusionmentioning

confidence: 99%

Search for Post-merger Gravitational Waves from the Remnant of the Binary Neutron Star Merger GW170817

Abbott¹,

Abbott²,

Abbott³

et al. 2017

ApJL

238

188

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show abstract

“…The former can easily compute sequences of non-rotating NSs, while the latter has been used to compute equilibrium configurations at the mass-shedding limit (Stergioulas 2003). The different EOSs were imported in LORENE in a table format either produced by using a piecewise polytropic approximation (APR4, Endrizzi et al 2016;H4, Kawamura et al 2016;MS1, Ciolfi et al 2017), provided by the EOS authors (SHT; Kastaun et al 2016), or given by the Compose project (GM1 6 ; Glendenning & Moszkowski 1991;Douchin & Haensel 2001). This large grid of models gives us, for each mass and EOS, a relation between the gravitational mass M e rd r 4 , 1…”

Section: Ns Modelsmentioning

confidence: 99%

The Fate of Neutron Star Binary Mergers

Piro

Giacomazzo

Perna

2017

ApJL

100

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Following merger, a neutron star (NS) binary can produce roughly one of three different outcomes: (1) a stable NS, (2) a black hole (BH), or (3) a supramassive, rotationally supported NS, which then collapses to a BH following angular momentum losses. Which of these fates occur and in what proportion has important implications for the electromagnetic transient associated with the mergers and the expected gravitational wave (GW) signatures, which in turn depend on the high density equation of state (EOS). Here we combine relativistic calculations of NS masses using realistic EOSs with Monte Carlo population synthesis based on the mass distribution of NS binaries in our Galaxy to predict the distribution of fates expected. For many EOSs, a significant fraction of the remnants are NSs or supramassive NSs. This lends support to scenarios in which a quickly spinning, highly magnetized NS may be powering an electromagnetic transient. This also indicates that it will be important for future GW observatories to focus on high frequencies to study the post-merger GW emission. Even in cases where individual GW events are too low in signal to noise to study the post merger signature in detail, the statistics of how many mergers produce NSs versus BHs can be compared with our work to constrain the EOS. To match short gamma-ray-burst (SGRB) X-ray afterglow statistics, we find that the stiffest EOSs are ruled out. Furthermore, many popular EOSs require a significant fraction of ∼60%-70% of SGRBs to be from NS-BH mergers rather than just binary NSs.

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“…bursts within the IGC paradigm [6,[38][39][40], and NS-NS (or NS-BH) binaries for short bursts, as widely accepted and confirmed by strong observational and theoretical evidences [12][13][14][15][16][17][18][19][20][21][22]. These paradigms have led to the classification of GRBs in seven different sub-classes (see figure 1).…”

Section: Discussionmentioning

confidence: 85%

“…Short bursts are associated to NS-NS or BH-NS mergers [12][13][14][15][16][17][18][19][20][21][22]: their host galaxies are of both early-and latetype, their localization with respect to the host galaxy often indicates a large offset [23][24][25][26][27][28][29] or a location of minimal star-forming activity with typical circumburst medium (CBM) densities of ∼ 10 −5 -10 −4 cm −3 , and no supernovae (SNe) have ever been associated to them.…”

Section: Introductionmentioning

confidence: 99%

What can we learn from GRBs?

et al. 2018

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Abstract. We review our recent results on the classification of long and short gamma-ray bursts (GRBs) in different subclasses. We provide observational evidences for the binary nature of GRB progenitors. For long bursts the induced gravitational collapse (IGC) paradigm proposes as progenitor a tight binary system composed of a carbon-oxygen core (CO core ) and a neutron star (NS) companion; the supernova (SN) explosion of the CO core triggers a hypercritical accretion process onto the companion NS. For short bursts a NS-NS merger is traditionally adopted as the progenitor. We also indicate additional sub-classes originating from different progenitors: (CO core )-black hole (BH), BH-NS, and white dwarf-NS binaries. We also show how the outcomes of the further evolution of some of these sub-classes may become the progenitor systems of other sub-classes.

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General relativistic magnetohydrodynamic simulations of binary neutron star mergers with the APR4 equation of state

Cited by 100 publications

References 54 publications

Search for Post-merger Gravitational Waves from the Remnant of the Binary Neutron Star Merger GW170817

Search for Post-merger Gravitational Waves from the Remnant of the Binary Neutron Star Merger GW170817

The Fate of Neutron Star Binary Mergers

What can we learn from GRBs?

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