A Broad Grid of 2D Kilonova Emission Models

Wollaeger, Ryan; Fryer, Chris L.; Chase, E. A.; Fontes, C. J.; Ristić, Marko; Hungerford, Aimee L.; Korobkin, Oleg; O’Shaughnessy, R.; Herring, Angela M.

doi:10.3847/1538-4357/ac0d03

Cited by 53 publications

(54 citation statements)

References 61 publications

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“…In this paper, we adopt an AT2017gfo-like model as our standard kilonova model to calculate the kilonova detectability of serendipitous and GW-triggered ToO observations. However, many theoretical works in the literature (e.g., Kasen et al 2013Kasen et al , 2017Kawaguchi et al 2020Kawaguchi et al , 2021Darbha & Kasen 2020;Korobkin et al 2021;Wollaeger et al 2021) show that BNS kilonova should be diverse which may depend on the mass ratio of binary and the nature of the merger remnant. The possible energy injection from the merger remnant, e.g., due to spindown of a post-merger magnetar (Yu et al 2013(Yu et al , 2018Metzger & Piro 2014;Ai et al 2018;Li et al 2018;Ren et al 2019) 3 or fall-back accretion onto the post-merger BH (Rosswog 2007;Ma et al 2018) could significantly increase the brightness of the kilonova.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. II. Optimal Search Strategy for Serendipitous Observations and Target-of-opportunity Observations of Gravitational-wave Triggers

Zhu¹,

Wu²,

Yang³

et al. 2021

Preprint

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In the second work of this series, we explore the optimal search strategy for serendipitous and gravitational-wave-triggered target-of-opportunity observations of kilonovae and optical short-duration gamma-ray burst (sGRB) afterglows from binary neutron star (BNS) mergers, assuming that cosmological kilonovae are AT2017gfo-like (but with viewing-angle dependence) and that the properties of afterglows are consistent with those of cosmological sGRB afterglows. A one-day cadence serendipitous search strategy with an exposure time of ∼ 30 s can always achieve an optimal search strategy of kilonovae and afterglows for various survey projects. We show that the optimal detection rates of the kilonova-dominated (afterglow-dominated) events are ∼ 0.2/0.5/0.8/20 yr −1 (∼ 500/300/600/3000 yr −1 ) for ZTF/Mephisto/WFST/LSST, respectively. A better search strategy for SiTian is to increase the exposure time. SiTian can find ∼ 5(6000) yr −1 kilonova-dominated (afterglow-dominated) events. We predict abundant off-axis orphan afterglows may be recorded in the survey database although not been identified. For target-of-opportunity observations, we simulate the maximum BNS gravitational-wave (GW) detection rates, which are ∼ 27/210/1800/2.0 × 10 5 yr −1 , in the networks of 2nd/2.5th/3rd(Voyager)/3rd(ET&CE)-generation GW detectors. In the upcoming 2nd-generation networks, follow-up observations with a limiting magnitude of m limit 22 − 23 mag can discover all EM signals from BNS GW events. Among these detected GW events, ∼ 60% events (∼ 16 yr −1 ) can detect clear kilonova signals, while afterglow-dominated events would account for the other ∼ 40% events (∼ 11 yr −1 ). In the 2.5th-and 3rd(Voyager)-generation era, the critical magnitudes for the detection of EM emissions from all BNS GW events would be ∼ 23.5 mag and ∼ 25 mag, respectively. Foreseeable optical survey projects cannot detect all EM signals of GW events detected during the ET&CE era.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. II. Optimal Search Strategy for Serendipitous Observations and Target-of-opportunity Observations of Gravitational-wave Triggers

Zhu¹,

Wu²,

Yang³

et al. 2021

Preprint

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“…the kilonova brightness may have a wide range of distribution and hence confirmed that kilonova emission should be diverse (Gompertz et al 2018;Ascenzi et al 2019;Rossi et al 2020;Rastinejad et al 2021). However, on one hand, kilonova emission is predicted to be highly viewing-angle-dependent (e.g., Kasen et al 2015;Martin et al 2015;Wollaeger et al 2018Wollaeger et al , 2021Barbieri et al 2019;Bulla 2019;Darbha & Kasen 2020;Zhu et al 2020;Korobkin et al 2021) so that one can only observe these kilonova candidates in sGRB afterglows when the line of sight is close to the jet axis. On the other hand, due to the scarce and ambiguous observational data, it is hard to use these limited data to model lightcurves of cosmological kilonovae 4 .…”

Section: Kilonova Emissionmentioning

confidence: 87%

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. I. Luminosity Function and Color Evolution

Zhu¹,

Yang²,

Zhang³

et al. 2021

Preprint

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In the first work of this series, we adopt an AT2017gfo-like viewing-angle-dependent kilonova model and the standard afterglow model with lightcurve distribution based on the cosmological short gammaray bursts afterglows to simulate the luminosity functions and color evolution of both kilonovae and optical afterglow emissions from binary neutron star mergers. Only a small fraction of (∼ 20%) on-axis afterglows are dimmer than the associated kilonovae at the kilonovae peak time. At a very large viewing angle, e.g., sin θ v 0.40, most kilonovae at the peak time would be much brighter than associated afterglows. Therefore, a large fractional of detectable kilonovae would be significantly polluted by associated afterglow emissions. We find that the maximum possible apparent magnitude for cosmological kilonovae is ∼ 27 − 28 mag. Afterglow emission has a wider luminosity function compared with kilonova emission. At brightness dimmer than ∼ 25 − 26 mag, according to their luminosity functions, the number of afterglows is much larger than that of kilonovae. Since the search depth of almost all the present and foreseeable survey projects is < 25 mag, the number of afterglow events detected via serendipitous observations would be much higher than that of kilonova events, consistent with the current observations. We find that it may be difficult to use the fading rate in a single band to directly identify kilonovae and afterglows among various fast-evolving transients by serendipitous surveys, especially if the observations have missed the peak time. However, the color evolution between optical and infrared bands can identify them, since their color evolution patterns are unique compared with those of other fast-evolving transients.

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“…Various types of parametrized, axisymmetric ejecta configurations have been employed in a series of papers by the Los Alamos group (Wollaeger et al 2018;Korobkin et al 2021;Wollaeger et al 2021, e.g.) using atomic-physics based opacities (Fontes et al 2020) and two different choices for the composition (Even et al 2020).…”

Section: Comparison With Previous Studiesmentioning

confidence: 99%

Dynamical ejecta of neutron star mergers with nucleonic weak processes II: Kilonova emission

Just,

Kullmann,

Goriely

et al. 2021

Preprint

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The majority of existing results for the kilonova (or macronova) emission from material ejected during a neutron-star (NS) merger is based on (quasi-)one-zone models or manually constructed toy-model ejecta configurations. In this study we present a kilonova analysis of the material ejected during the first ∼ 10 ms of a NS merger, called dynamical ejecta, using directly the outflow trajectories from general relativistic smoothed-particle hydrodynamics simulations including a sophisticated neutrino treatment and the corresponding nucleosynthesis results, which have been presented in Part I of this study. We employ a multi-dimensional two-moment radiation transport scheme with approximate M1 closure to evolve the photon field and use a heuristic prescription for the opacities found by calibration with atomic-physics based reference results. We find that the photosphere is generically ellipsoidal but augmented with small-scale structure and produces emission that is about 1.5-3 times stronger towards the pole than the equator. The kilonova typically peaks after 0.7 − 1.5 days in the near-infrared frequency regime with luminosities between 3 − 7 × 10 40 erg s −1 and at photospheric temperatures of 2.2 − 2.8 × 10 3 K. A softer equation of state or higher binary-mass asymmetry leads to a longer and brighter signal. Significant variations of the light curve are also obtained for models with artificially modified electron fractions, emphasizing the importance of a reliable neutrino-transport modeling. None of the models investigated here, which only consider dynamical ejecta, produces a transient as bright as AT2017gfo. The near-infrared peak of our models is incompatible with the early blue component of AT2017gfo.

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A Broad Grid of 2D Kilonova Emission Models

Cited by 53 publications

References 61 publications

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. II. Optimal Search Strategy for Serendipitous Observations and Target-of-opportunity Observations of Gravitational-wave Triggers

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. II. Optimal Search Strategy for Serendipitous Observations and Target-of-opportunity Observations of Gravitational-wave Triggers

Kilonova and Optical Afterglow from Binary Neutron Star Mergers. I. Luminosity Function and Color Evolution

Dynamical ejecta of neutron star mergers with nucleonic weak processes II: Kilonova emission

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