Modeling dynamical ejecta from binary neutron star mergers and implications for electromagnetic counterparts

Dietrich, Tim; Ujevic, Maximiliano

doi:10.1088/1361-6382/aa6bb0

Cited by 148 publications

(185 citation statements)

References 57 publications

(199 reference statements)

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“…The fitting parameters are: the opacity of the ejecta κ = 10 cm 2 g −1 , the ejecta velocity v ej = 0.29c (c is the speed of light), and the mass of the ejecta M ej = 0.0105 M . These numbers are consistent with typical values obtained by numerical simulations of BNS mergers [48]. Note that the opacity of the r-process ejecta with the lanthanides, κ = 10 − 100 cm 2 g −1 , is much higher than the opacity for iron-peak elements.…”

Section: Theoretical Interpretationsupporting

confidence: 90%

“…t c is the critical time, after which (t > t c ) the ejecta becomes transparent. [47] and [48] found that the bolometric light curve of this analytic model function can reasonably match the results of the radiation-transfer simulation performed in [21].…”

Section: Theoretical Interpretationmentioning

confidence: 54%

“…here we adopt˙ 0 = 1.58 × 10 10 erg g −1 s −1 and the thermalization efficiency th = 0.5 following [48]. t c is the critical time, after which (t > t c ) the ejecta becomes transparent.…”

Section: Theoretical Interpretationmentioning

confidence: 99%

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Optical observations of LIGO source GW 170817 by the Antarctic Survey Telescopes at Dome A, Antarctica

Andreoni

et al. 2017

Science Bulletin

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The LIGO detection of gravitational waves (GW) from merging black holes in 2015 marked the beginning of a new era in observational astronomy. The detection of an electromagnetic signal from a GW source is the critical next step to explore in detail the physics involved. The Antarctic Survey Telescopes (AST3), located at Dome A, Antarctica, is uniquely situated for rapid response time-domain astronomy with its continuous night-time coverage during the austral winter. We report optical observations of the GW source (GW 170817) in the nearby galaxy NGC 4993 using AST3. The data show a rapidly fading transient at around 1 day after the GW trigger, with the i-band magnitude declining from 17.23 ± 0.13 magnitude to 17.72 ± 0.09 magnitude in ∼ 1.8 hour. The brightness and time evolution of the optical transient associated with GW 170817 are broadly consistent with the predictions of models involving merging binary neutron stars. We infer from our data that the merging process ejected about ∼ 10 −2 solar mass of radioactive material at a speed of up to 30% the speed of light.

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Section: Theoretical Interpretationsupporting

confidence: 90%

Section: Theoretical Interpretationmentioning

confidence: 54%

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Optical observations of LIGO source GW 170817 by the Antarctic Survey Telescopes at Dome A, Antarctica

Andreoni

et al. 2017

Science Bulletin

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“…Kasen et al (2013) and found that the opacity of r-process ejecta, particularly the lanthanides, is much higher than that for Fe-peak elements, with κ ∼ 10 − 100 cm 2 g −1 . Kawaguchi et al (2016) and Dietrich & Ujevic (2017) found that the bolometric light curve of a kilonova in the analytic model mentioned above can well match the results of radiation-transfer simulations performed in Tanaka & Hotokezaka (2013).…”

Section: Kilonovaesupporting

confidence: 53%

“…The bolometric luminosity of kilonova is approximated by (Kawaguchi et al 2016;Dietrich & Ujevic 2017)…”

Section: Kilonovaementioning

confidence: 99%

Afterglows and Kilonovae Associated with Nearby Low-luminosity Short-duration Gamma-Ray Bursts: Application to GW170817/GRB 170817A

Xiao

Liu

Dai

et al. 2017

ApJL

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Very recently, the gravitational wave (GW) event GW170817 was discovered to be associated with the short gamma-ray burst (GRB) 170817A. Multi-wavelength follow-up observations were carried out, and X-ray, optical and radio counterparts to GW170817 were detected. The observations undoubtedly indicate that GRB170817A originates from a binary neutron star (BNS) merger. However, the GRB falls into the low-luminosity class which could have a higher statistical occurrence rate and detection probability than the normal (high-luminosity) class. This implies a possibility that GRB170817A is intrinsically powerful but we are off-axis and only observe its side emission. In this paper, we provide a timely modeling of the multi-wavelength afterglow emission from this GRB and the associated kilonova signal from the merger ejecta, under the assumption of a structured jet, a two-component jet, and an intrinsically less-energetic quasi-isotropic fireball respectively. Comparing the afterglow properties with the multi-wavelength follow-up observations, we can distinguish between these three models. Furthermore, a few model parameters (e.g., the ejecta mass and velocity) can be constrained.

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Heavy Elements and Electromagnetic Transients from Neutron Star Mergers

Rosswog

Korobkin

2022

Annalen der Physik

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Compact binary mergers involving neutron stars can eject a fraction of their mass to space. Being extremely neutron rich, this material undergoes rapid neutron capture nucleosynthesis, and the resulting radioactivity powers fast, short‐lived electromagnetic transients known as kilonova or macronova. Such transients are exciting probes of the most extreme physical conditions and their observation signals the enrichment of the Universe with heavy elements. Here the current understanding of the mass ejection mechanisms, the properties of the ejecta, and the resulting radioactive transients are reviewed. The first well‐observed event in the aftermath of GW170817 delivered a wealth of insights, but much of today's picture of such events is still based on a patchwork of theoretical studies. Apart from summarizing the current understanding, questions where no consensus has been reached yet are also pointed out, and possible directions for the future research are sketched. In an appendix, a publicly available heating rate library based on the WinNet nuclear reaction network is described, and a simple fit formula to alleviate the implementation in hydrodynamic simulations is provided.

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Modeling dynamical ejecta from binary neutron star mergers and implications for electromagnetic counterparts

Cited by 148 publications

References 57 publications

Optical observations of LIGO source GW 170817 by the Antarctic Survey Telescopes at Dome A, Antarctica

Optical observations of LIGO source GW 170817 by the Antarctic Survey Telescopes at Dome A, Antarctica

Afterglows and Kilonovae Associated with Nearby Low-luminosity Short-duration Gamma-Ray Bursts: Application to GW170817/GRB 170817A

Heavy Elements and Electromagnetic Transients from Neutron Star Mergers

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