Light Curves and Spectra from a Unimodal Core-collapse Supernova

Wollaeger, Ryan; Hungerford, Aimee L.; Fryer, Chris L.; Wollaber, Allan B.; Rossum, Daniel R. van; Even, Wesley

doi:10.3847/1538-4357/aa82bd

Cited by 16 publications

(18 citation statements)

References 125 publications

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“…Our analysis is somewhat different from that of Wollaeger et al (2017) and Barnes et al (2017), who also conduct non-spherically-symmetric hydrodynamical simulations and then predict band-dependent light curves based on the result. Whereas these authors assume a state of homologous free expansion and conduct Monte Carlo radiative transfer within the ejecta, accounting for radioactive heating, our approach addresses the emission of shock-deposited heat before homologous expansion is established.…”

Section: Summary and Discussionmentioning

confidence: 66%

Aspherical Supernovae: Effects on Early Light Curves

Afsariardchi

Matzner

2018

ApJ

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Early light from core-collapse supernovae, now detectable in high-cadence surveys, holds clues to a star and its environment just before it explodes. However, effects that alter the early light have not been fully explored. We highlight the possibility of non-radial flows at the time of shock breakout. These develop in sufficiently non-spherical explosions if the progenitor is not too diffuse. When they do develop, non-radial flows limit ejecta speeds and cause ejecta-ejecta collisions. We explore these phenomena and their observational implications, using global, axisymmetric, non-relativistic FLASH simulations of simplified polytropic progenitors, which we scale to representative stars. We develop a method to track photon production within the ejecta, enabling us to estimate band-dependent light curves from adiabatic simulations. Immediate breakout emission becomes hidden as an oblique flow develops. Non-spherical effects lead the shock-heated ejecta to release a more constant luminosity at a higher, evolving color temperature at early times, effectively mixing breakout light with the early light curve. Collisions between non-radial ejecta thermalize a small fraction of the explosion energy; we address emission from these collisions in a subsequent paper.

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Section: Summary and Discussionmentioning

confidence: 66%

Aspherical Supernovae: Effects on Early Light Curves

Afsariardchi

Matzner

2018

ApJ

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“…Originally intended for supernova transients (van Rossum et al 2016;Kozyreva et al 2017;Wollaeger et al 2017), SuperNu has been applied to modeling kilonovae in 1D and 2D axisymmetric geometry (Kasliwal et al 2017b;Troja et al 2017;Tanvir et al 2017;Evans et al 2017;Wollaeger et al 2018Wollaeger et al , 2019Even et al 2019). These studies varied the mass and velocity of wind and dynamical ejecta components but always assumed a spherical wind superimposed with ejecta from SPH simulations (Rosswog et al 2014).…”

Section: Radiative Transfer Modelingmentioning

confidence: 99%

Axisymmetric Radiative Transfer Models of Kilonovae

Korobkin,

Wollaeger,

Fryer

et al. 2020

Preprint

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The detailed observations of GW170817 proved for the first time directly that neutron star mergers are a major production site of heavy elements. The observations could be fit by a number of simulations that qualitatively agree, but can quantitatively differ (e.g. in total r-process mass) by an order of magnitude. We categorize kilonova ejecta into several typical morphologies motivated by numerical simulations, and apply a radiative transfer Monte Carlo code to study how the geometric distribution of the ejecta shapes the emitted radiation. We find major impacts on both spectra and light curves. The peak bolometric luminosity can vary by two orders of magnitude and the timing of its peak by a factor of five. These findings provide the crucial implication that the ejecta masses inferred from observations are uncertain by at least an order of magnitude. Mixed two-component models with lanthanide-rich ejecta are particularly sensitive to geometric distribution. A subset of mixed models shows very strong viewing angle dependence due to lanthanide "curtaining", which persists even if the relative mass of lanthanide-rich component is small. The angular dependence is weak in the rest of our models, but different geometric combinations of the two components lead to a highly diverse set of light curves. We identify geometry-dependent P Cygni features in late spectra that directly map out strong lines in the simulated opacity of neodymium, which can help to constrain the ejecta geometry and to directly probe the r-process abundances.

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“…In fact, there have been several efforts to evaluate the opacity from atomic models. The earliest works attempted the calculation for only a few representative elements (Kasen et al 2013;Tanaka & Hotokezaka 2013;Fontes et al 2017;Wollaeger et al 2017;Tanaka et al 2018), assuming that the overall ejecta opacity can be reflected by these elements. More recently, atomic opacity data for all lanthanides (Z = 58 − 70, Kasen et al 2017;Fontes et al 2020) and finally all the r-process elements (Z = 31 − 88, Tanaka et al 2020) have been calculated.…”

Section: Introductionmentioning

confidence: 99%

Simulations of early kilonova emission from neutron star mergers

Banerjee,

Tanaka,

Kawaguchi

et al. 2020

Preprint

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We present radiative transfer simulations for blue kilonovae hours after neutron star (NS) mergers by performing detailed opacity calculations for the first time. We calculate atomic structures and opacities of highly ionized elements (up to the tenth ionization) with atomic number Z = 20 − 56. We find that the bound-bound transitions of heavy elements are the dominant source of the opacities in the early phase (t < 1 day after the merger), and that the ions with a half-closed electron shell provide the highest contributions. The Planck mean opacity for lanthanide-free ejecta (with electron fraction of Y e = 0.30 − 0.40) can only reach around κ ∼ 0.5 − 1 cm 2 g −1 at t = 0.1 day, whereas that increases up to κ ∼ 5 − 10 cm 2 g −1 at t = 1 day. The spherical ejecta model with an ejecta mass of M ej = 0.05M ⊙ gives the bolometric luminosity of ∼ 2 × 10 42 erg s −1 at t ∼ 0.1 day. We confirm that the existing bolometric and multi-color data of GW170817 can be naturally explained by the purely radioactive model. The expected early UV signals reach 20.5 mag at t ∼ 4.3 hours for sources even at 200 Mpc, which is detectable by the facilities such as Swift and the Ultraviolet Transient Astronomy Satellite (ULTRASAT). The early-phase luminosity is sensitive to the structure of the outer ejecta, as also pointed out by Kasen et al. (2017). Therefore, the early UV observations give strong constraints on the structure of the outer ejecta as well as the presence of a heating source besides r-process nuclei.

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Light Curves and Spectra from a Unimodal Core-collapse Supernova

Cited by 16 publications

References 125 publications

Aspherical Supernovae: Effects on Early Light Curves

Aspherical Supernovae: Effects on Early Light Curves

Axisymmetric Radiative Transfer Models of Kilonovae

Simulations of early kilonova emission from neutron star mergers

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