The Physics of Kilonovae

Barnes, Jennifer

doi:10.3389/fphy.2020.00355

Cited by 16 publications

(7 citation statements)

References 115 publications

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“…The ejection is anisotropic with neutron-rich, dynamical ejecta in the equatorial plane, where the formation of lanthanides leads to a large opacity while a relatively neutron-poor wind of lower opacity is blown in the polar direction (Fernández & Metzger 2016;Metzger 2019;Barnes 2020). This wind is expected to be present when a short-lived massive neutron star is formed before collapsing to a black hole, but probably not in the case of a direct collapse.…”

Section: Kilonova Magnitude Dependence To Viewing Anglementioning

confidence: 99%

Prospects for kilonova signals in the gravitational-wave era

Mochkovitch

Daigne

Duque

et al. 2021

A&A

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The binary neutron star merger gravitational-wave signal GW170817 was followed by three electromagnetic counterparts, including a kilonova arising from the radioactivity of freshly synthesized r-process elements in ejecta from the merger. Finding kilonovae after gravitational-wave triggers is crucial for (i) the search for further counterparts, such as the afterglow, (ii) probing the diversity of kilonovae and their dependence on the system’s inclination angle, and (iii) building a sample for multi-messenger cosmology. During the third observing run of the gravitational-wave interferometer network, no kilonova counterpart was found. We aim to predict the expected population of detectable kilonova signals for the upcoming O4 and O5 observing runs of the LIGO-Virgo-KAGRA instruments. Using a simplified criterion for gravitational-wave detection and a simple GW170817-calibrated model for the kilonova peak magnitude, we determine the rate of kilonovae in reach of follow-up campaigns and their distributions in magnitude for various bands. We briefly consider the case of GW190425, the only binary neutron star merger confirmed since GW170817, and obtain constraints on its inclination angle from the non-detection of its kilonova, assuming the source was below the follow-up thresholds. We also show that non-gravitational-wave-triggered kilonovae can be a numerous class of sources in future surveys and briefly discuss associations with short bright gamma-ray bursts. We finally discuss the detection of the jetted outflow afterglow in addition to the kilonova.

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Section: Kilonova Magnitude Dependence To Viewing Anglementioning

confidence: 99%

Prospects for kilonova signals in the gravitational-wave era

Mochkovitch

Daigne

Duque

et al. 2021

A&A

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“…The kilonova magnitude at the peak depends on the distributions of mass, velocity and composition of the ejected material and on the viewing conditions: distance and viewing angle. The ejection is anisotropic with a neutron-rich, dynamical ejecta in the equatorial plane, where the formation of lanthanides leads to a large opacity while a relatively neutron-poor wind of lower opacity is blown in the polar direction (Fernández & Metzger 2016;Metzger 2019;Barnes 2020). This wind is expected to be present when a short-lived massive neutron star is formed before collapsing to a black hole, but probably not in the case of a direct collapse.…”

Section: Kilonova Magnitude Dependence To Viewing Anglementioning

confidence: 99%

Prospects for kilonova signals in the gravitational-wave era

Mochkovitch,

Daigne,

Duque

et al. 2021

Preprint

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The binary neutron star merger gravitational-wave signal GW170817 was followed by three electromagnetic counterparts, of which a kilonova arising from the radioactivity of freshly synthesized r-process elements in ejecta from the merger. Finding kilonovae after gravitational-wave triggers is crucial (i) to the search for further counterparts such as the afterglow, (ii) to probe the diversity of kilonovae and their dependence on the system's inclination angle (iii) to build a sample for multimessenger cosmology. During the third observing run of the gravitational-wave interferometer network, no kilonova counterpart was found. We aim to predict the expected population of detectable kilonova signals for the upcoming O4 and O5 observing runs of the LIGO-Virgo-Kagra instruments. Using a a simplified criterion for gravitational-wave detection and a simple GW170817-calibrated model for the kilonova peak magnitude, we determine the rate of kilonovae in reach of follow-up campaigns and their distributions in magnitude for various bands. We briefly consider the case of GW190425, the only confirmed binary neutron star merger since GW170817, and obtain constraints on its inclination angle from the non-detection of its kilonova, assuming the source was below the follow-up thresholds. We also show that non gravitational-wave-triggered kilonovae can be a numerous class of sources in the future surveys and briefly discuss associations with short bright gamma-ray bursts. We finally discuss the detection of the jetted outflow afterglow in addition to the kilonova, and confirm former conclusions on the rareness of such counterparts in future observations.

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“…In addition to demonstrating the long-theorized viability of NSMs as r -process sites (e.g., Lattimer & Schramm 1974;Symbalisty & Schramm 1982;Eichler et al 1989;Freiburghaus et al 1999), kn170817 provided an unprecedentedly detailed picture of the various environments in which the r -process may occur following a merger (Drout et al 2017;Cowperthwaite et al 2017;Kilpatrick et al 2017;Tanvir et al 2017, among others). In particular, spectral analysis (e.g., Chornock et al 2017;Kasen et al 2017;and Tanaka et al 2017; see Siegel (2019) and Barnes (2020) for reviews) pointed to accretion disk outflows (Metzger et al 2008;Fernández & Metzger 2013;Perego et al 2014;Just et al 2015;Siegel & Metzger 2017;Fujibayashi et al 2018;Fernández et al 2019) as the locus of the heaviest element production. (However, see Waxman et al (2018) for an alternative interpretation.)…”

Section: Introductionmentioning

confidence: 99%

Signatures of R-process Enrichment in Supernovae from Collapsars

Barnes¹,

Metzger²

2022

Preprint

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Despite recent progress, the astrophysical channels responsible for rapid neutron capture (r -process) nucleosynthesis remain an unsettled question. Observations of kilonovae following gravitational wavedetected neutron star mergers established mergers as one site of the r -process, but additional sources may be needed to fully explain r -process enrichment in the Universe. One intriguing possibility is that rapidly rotating massive stars undergoing core collapse launch r -process-rich outflows off the accretion disks formed from their infalling matter. In this scenario, r -process winds comprise one component of the supernova (SN) ejecta produced by "collapsar" explosions. We present the first systematic study of the effects of r -process enrichment on the emission from collapsar-generated SNe. We semi-analytically model r -process SN emission from explosion out to late times, and determine its distinguishing features. The ease with which r -process SNe can be identified depends on how effectively wind material mixes into the initially r -process-free outer layers of the ejecta. In many cases, enrichment produces a near infrared (NIR) excess that can be detected within ∼75 days of explosion. We also discuss optimal targets and observing strategies for testing the r -process collapsar theory, and find that frequent monitoring of optical and NIR emission from high-velocity SNe in the first few months after explosion offers a reasonable chance of success while respecting finite observing resources. Such early identification of r -process collapsar candidates also lays the foundation for nebular-phase spectroscopic follow-up in the near-and mid-infrared, for example with the James Webb Space Telescope.

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The Physics of Kilonovae

Cited by 16 publications

References 115 publications

Prospects for kilonova signals in the gravitational-wave era

Prospects for kilonova signals in the gravitational-wave era

Prospects for kilonova signals in the gravitational-wave era

Signatures of R-process Enrichment in Supernovae from Collapsars

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