The unpolarized macronova associated with the gravitational wave event GW 170817

Covino, S.; Wiersema, K.; Fan, Yi‐Zhong; Toma, Kenji; Higgins, A. B.; Melandri, A.; D’Avanzo, P.; Mundell, C. G.; Palazzi, E.; Tanvir, N. R.; Bernardini, M. G.; Branchesi, M.; Brocato, E.; Campana, S.; Alighieri, S. di Serego; Götz, D.; Fynbo, J. P. U.; Gao, Wei-Hong; Gomboc, A.; Gompertz, B.; Greiner, J.; Hjorth, J.; Jin, Zhi-Ping; Kaper, L.; Klose, S.; Kobayashi, S.; Kopač, D.; Kouveliotou, C.; Levan, A. J.; Mao, J. R.; Malesani, D.; Pian, E.; Rossi, A.; Salvaterra, R.; Starling, R. L. C.; Steele, I. A.; Tagliaferri, G.; Troja, E.; Horst, A. J. van der; Wijers, R. A. M. J.

doi:10.1038/s41550-017-0285-z

Cited by 92 publications

(71 citation statements)

References 34 publications

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“…The discovery, about 12 hours after the GBM trigger, of the associated optical transient AT2017gfo (Coulter et al 2017;Valenti et al 2017) triggered an intense ultraviolet, optical and infrared (UVOIR) follow up campaign (e.g. Andreoni et al 2017;Arcavi et al 2017;Chornock et al 2017;Covino et al 2017;Díaz et al 2017;Drout et al 2017;Evans et al 2017;Hal-1 Similar results were obtained by an independent analysis by Zhang et al (2018) linan et al 2017; Pian et al 2017;Pozanenko et al 2018;Smartt et al 2017;Utsumi et al 2017) -whose results have been collected and homogenized in Villar et al (2017) -which characterised with unprecedented details the emission and color evolution of the first ever spectroscopically confirmed (e.g. Pian et al 2017;Cowperthwaite et al 2017;Gall et al 2017;Kilpatrick et al 2017;McCully et al 2017;Nicholl et al 2017;Smartt et al 2017) kilonova (KN), i.e.…”

Section: Introductionmentioning

confidence: 99%

On-axis view of GRB 170817A

Salafia

Ghirlanda

Ascenzi

et al. 2019

A&A

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The peculiar short gamma-ray burst GRB 170817A has been firmly associated to the gravitational wave event GW170817, which has been unaninmously interpreted as due to the coalescence of a double neutron star binary. The unprecedented behaviour of the non-thermal afterglow led to a debate about its nature, which was eventually settled by high-resolution VLBI observations, which strongly support the off-axis structured jet scenario. Using information on the jet structure derived from multi-wavelength fitting of the afterglow emission and of the apparent VLBI image centroid motion, we compute the appearance of a GRB 170817A-like jet as seen by an on-axis observer and we compare it to the previously observed population of SGRB afterglows and prompt emission events. We find that the intrinsic properties of the GRB 170817A jet are representative of a typical event in the SGRB population, hinting at a quasi-universal jet structure. The diversity in the SGRB afterglow population could therefore be ascribed in large part to extrinsic (redshift, density of the surrounding medium, viewing angle) rather than intrinsic properties. Although more uncertain, the comparison can be extended to the prompt emission properties, leading to similar conclusions.

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Section: Introductionmentioning

confidence: 99%

On-axis view of GRB 170817A

Salafia

Ghirlanda

Ascenzi

et al. 2019

A&A

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“…[3][4][5][6][7][8][9][10][11][12][13][14]). These observations show that the emission properties are largely consistent with the macronova/kilonova model [15,16], suggesting that high-velocity, neutronrich matter of mass 0.01-0.1M ejected from the neutron-star mergers radioactively shines through the rprocess nucleosynthesis [17,18] in the optical-IR bands for 0.5-20 days after the merger, and that the spectrum is broadly consistent with the quasi-thermal spectrum with significant reddening.…”

Section: Introductionmentioning

confidence: 99%

Modeling GW170817 based on numerical relativity and its implications

et al. 2017

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Gravitational-wave observation together with a large number of electromagnetic observations shows that the source of the latest gravitational-wave event, GW170817, detected primarily by advanced LIGO, is the merger of a binary neutron star. We attempt to interpret this observational event based on our results of numerical-relativity simulations performed so far paying particular attention to the optical and infra-red observations. We finally reach a conclusion that this event is described consistently by the presence of a long-lived hypermassive or supramassive neutron star as the merger remnant, because (i) significant contamination by lanthanide elements along our line of sight to this source can be avoided by the strong neutrino irradiation from it and (ii) it could play a crucial role to produce an ejecta component of appreciable mass with fast motion in the postmerger phase. We also point out that (I) the neutron-star equation of state has to be sufficiently stiff (i.e., the maximum mass of cold spherical neutron stars, Mmax, has to be appreciably higher than 2M ) in order that a long-lived massive neutron star can be formed as the merger remnant for the binary systems of GW170817, for which the initial total mass is 2.73M and (II) no detection of relativistic optical counterpart suggests a not-extremely high value of Mmax approximately as 2.15-2.25M .

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“…In the following, we show the time scale of visibility of a kilonova by taking AT 2017gfo as a typical kilonova. AT 2017gfo with an absolute peak magnitude of M = −15.8±0.1 and a r-band decline rate of 1.1 mag/d offers the unique opportunity to study kilonova emission that was plausibly not polluted by the gamma ray burst (GRB) afterglow emission (Valenti, et al 2017;Covino, et al 2017). We put AT 2017gfo at a distance of 10 kpc and compare it with some typical supernovae at 15 kpc (see detailed reason why 10 kpc and 15 kpc are adopted in Section.…”

Section: The Guest Star Of Ad 1163mentioning

confidence: 99%

G4.8+6.2, a possible kilonova remnant?

Liu

Zou

Jiang

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

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Kilonova explosions typically release ∼ 10 50−51 erg in kinetic energy, which is sufficient to constitute a kilonova remnant (KNR); however, it has not yet been confirmed. In this work, we investigate the probable association between G4.8+6.2 and the guest star of AD 1163, which is recorded by the Korea ancient astronomers. Although the evidence available is insufficient to draw a definite conclusion, it is at least theoretically self-consistent that the guest star of AD 1163 was a historical kilonova associated with G4.8+6.2, considering the possible short visible timescale of AD 1163, the relatively high Galactic latitude of G4.8+6.2, and that G4.8+6.2 is spatially coincident with the guest star of AD 1163. Further observation of G4.8+6.2 is needed to test our hypothesis. If our interpretation is correct, our results indicate that young KNRs should have a large diameter and low surface brightness, unlike other young supernova remnants.

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The unpolarized macronova associated with the gravitational wave event GW 170817

Cited by 92 publications

References 34 publications

On-axis view of GRB 170817A

On-axis view of GRB 170817A

Modeling GW170817 based on numerical relativity and its implications

G4.8+6.2, a possible kilonova remnant?

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