Origin of the heavy elements in binary neutron-star mergers from a gravitational-wave event

Kasen, Daniel; Metzger, Brian; Barnes, Jennifer; Quataert, Eliot; Ramírez-Ruiz, E.

doi:10.1038/nature24453

Cited by 1,150 publications

(1,344 citation statements)

References 66 publications

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“…The light-curve properties were interpreted as being produced by dynamical ejecta from the merger and secular ejecta from the merger remnant. The estimated ejecta mass is in the range 0.03 to 0.05 M (Cowperthwaite et al 2017;Kasen et al 2017;Nicholl et al 2017;Chornock et al 2017;Drout et al 2017;Smartt et al 2017;Kasliwal et al 2017;Kilpatrick et al 2017;Tanvir et al 2017;Tanaka et al 2017), which even for asymmetric binaries lies near the high end of the theoretical range expected from simulations. This can be interpreted as tentative evidence for a delayed/no collapse in GW170817 because this merger outcome tends to produce larger ejecta masses as compared to a direct collapse (Bauswein et al 2013b;Hotokezaka et al 2013;Fernández & Metzger 2013;Metzger & Fernández 2014;Perego et al 2014;Siegel et al 2014;Wanajo et al 2014;Just et al 2015;Sekiguchi et al 2016).…”

Section: Observationsmentioning

confidence: 99%

“…Our constraint only relies on the measured binary mass of GW170817 and the evidence for a delayed/no collapse in this event as suggested by its electromagnetic emission (e.g. Kasen et al 2017;Metzger 2017). In the case of a delayed/no collapse the measured total binary mass of GW170817 provides a lower bound on the threshold mass for direct BH formation,…”

Section: Introductionmentioning

confidence: 99%

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Neutron-star Radius Constraints from GW170817 and Future Detections

Bauswein

Just

Janka

et al. 2017

ApJL

669

629

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We introduce a new, powerful method to constrain properties of neutron stars (NSs). We show that the total mass of GW170817 provides a reliable constraint on the stellar radius if the merger did not result in a prompt collapse as suggested by the interpretation of associated electromagnetic emission. The radius R 1.6 of nonrotating NSs with a mass of 1.6 M can be constrained to be larger than 10.68−0.04 km, and the radius R max of the nonrotating maximum mass configuration must be larger than 9.60 +0.14 −0.03 km. We point out that detections of future events will further improve these constraints. Moreover, we show that a future event with a signature of a prompt collapse of the merger remnant will establish even stronger constraints on the NS radius from above and the maximum mass M max of NSs from above. These constraints are particularly robust because they only require a measurement of the chirp mass and a distinction between prompt and delayed collapse of the merger remnant, which may be inferred from the electromagnetic signal or even from the presence/absence of a ringdown gravitational-wave (GW) signal. This prospect strengthens the case of our novel method of constraining NS properties, which is directly applicable to future GW events with accompanying electromagnetic counterpart observations. We emphasize that this procedure is a new way of constraining NS radii from GW detections independent of existing efforts to infer radius information from the late inspiral phase or postmerger oscillations, and it does not require particularly loud GW events.

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Section: Observationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Neutron-star Radius Constraints from GW170817 and Future Detections

Bauswein

Just

Janka

et al. 2017

ApJL

669

629

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“…Indeed, the opposite view of interpreting the blue component as due to the dynamical ejecta exists in the literature (e.g. Kasen et al 2017;Nicholl et al 2017).…”

Section: Introductionmentioning

confidence: 99%

“…The optical/IR counterpart of GW170817 indeed showed two distinct blue and red components (Evans et al 2017;Drout et al 2017;Nicholl et al 2017;Smartt et al 2017;Arcavi et al 2017;Kasen et al 2017;Cowperthwaite et al 2017;Kilpatrick et al 2017;Villar et al 2017). Fitting the light curve, one could obtain the properties for both components, such as their velocities, opacities, and especially the masses of the two components.…”

Section: Introductionmentioning

confidence: 99%

A More Stringent Constraint on the Mass Ratio of Binary Neutron Star Merger GW170817

Cao

Zhang

2017

ApJL

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Recently, the LIGO-Virgo collaboration reported their first detection of gravitational wave (GW) signals from a low mass compact binary merger GW170817, which is most likely due to a double neutron star (NS) merger. With the GW signals only, the chirp mass of the binary is precisely constrained to 1.188 +0.004 −0.002 M , but the mass ratio is loosely constrained in the range 0.4 − 1, so that a very rough estimation of the individual NS masses (1.36 M < M 1 < 2.26 M and 0.86 M < M 2 < 1.36 M ) was obtained. Here we propose that if one can constrain the dynamical ejecta mass through performing kilonova modeling of the optical/IR data, by utilizing an empirical relation between the dynamical ejecta mass and the mass ratio of NS binaries, one may place a more stringent constraint on the mass ratio of the system. For instance, considering that the red "kilonova" component is powered by the dynamical ejecta, we reach a tight constraint on the mass ratio in the range of 0.46 − 0.59. Alternatively, if the blue "kilonova" component is powered by the dynamical ejecta, the mass ratio would be constrained in the range of 0.53 − 0.67. Overall, such a multi-messenger approach could narrow down the mass ratio of GW170817 system to the range of 0.46 − 0.67, which gives a more precise estimation of the individual NS mass than pure GW signal analysis, i.e. 1.61 M < M 1 < 2.11 M and 0.90 M < M 2 < 1.16 M .

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“…For instance, the detection of a short gamma ray burst (GRB) 1.7 seconds after GW170817 [24][25][26], and subsequent kilonova [27][28][29][30][31][36][37][38][39][40][41][42][43][44], confirmed that BNS mergers are a progenitor of these events. Lanthanide signatures in the kilonova light curves also showed BNS mergers to be a major site for nucleosynthesis of elements heavier than iron [40,44,47,48]. Furthermore the measurements of the EM redshift and, from the GW signal, the luminosity distance, allowed an independent estimate of the Hubble constant to be made [49], thus demonstrating a thirty year old prediction [50].…”

Section: Introductionmentioning

confidence: 99%

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Mills¹,

Tiwari²,

Fairhurst³

2018

Phys. Rev. D

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The observation of gravitational wave signals from binary black hole and binary neutron star mergers has established the field of gravitational wave astronomy. It is expected that future networks of gravitational wave detectors will possess great potential in probing various aspects of astronomy. An important consideration for successive improvement of current detectors or establishment on new sites is knowledge of the minimum number of detectors required to perform precision astronomy. We attempt to answer this question by assessing the ability of future detector networks to detect and localize binary neutron stars mergers on the sky. Good localization ability is crucial for many of the scientific goals of gravitational wave astronomy, such as electromagnetic follow-up, measuring the properties of compact binaries throughout cosmic history, and cosmology. We find that although two detectors at improved sensitivity are sufficient to get a substantial increase in the number of observed signals, at least three detectors of comparable sensitivity are required to localize majority of the signals, typically to within around 10 deg 2 -adequate for follow-up with most wide field of view optical telescopes.

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Origin of the heavy elements in binary neutron-star mergers from a gravitational-wave event

Cited by 1,150 publications

References 66 publications

Neutron-star Radius Constraints from GW170817 and Future Detections

Neutron-star Radius Constraints from GW170817 and Future Detections

A More Stringent Constraint on the Mass Ratio of Binary Neutron Star Merger GW170817

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

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