Numerical simulations of superluminous supernovae of type IIn

Dessart, Luc; Audit, E.; Hillier, D. J.

doi:10.1093/mnras/stv609

Cited by 116 publications

(177 citation statements)

References 57 publications

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“…Although the BB fits give a good agreement with the observed SED, this may, especially at later epochs, underestimate the luminosity and also the radius of the hot component. This is illustrated by the simulation of SN 2010jl in Dessart et al (2015, their Fig. 13), where the model has a considerable UV contribution compared to a BB fit of only the optical range.…”

Section: Seds and Constructing The Bolometric Light Curvementioning

confidence: 93%

“…Here, we model this by a temperature decreasing as T e ∝ r −0.4 from the shock, but the line profile is not very sensitive to this assumption. Also for other parameters, such as the bound-free opacity, we use the model by Dessart et al (2015) as a guide. It is important to note, however, that this model was used for a relatively low ejecta mass of 9.8 M , while a more massive ejecta may give different parameters.…”

Section: Modeling Of the Spectral Linesmentioning

confidence: 99%

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The Carnegie Supernova Project II

Taddia

Stritzinger

Fransson

et al. 2020

A&A

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We present ultra-violet (UV) to mid-infrared (MIR) observations of the long-lasting Type IIn supernova (SN) 2013L obtained by the Carnegie Supernova Project II (CSP-II) beginning two days after discovery and extending until +887 days (d). The SN reached a peak r-band absolute magnitude of ≈ −19 mag and an even brighter UV peak, and its light curve evolution resembles that of SN 1988Z. The spectra of SN 2013L are dominated by hydrogen emission features, characterized by three components attributed to different emission regions. A unique feature of this Type IIn SN is that, apart from the first epochs, the blue shifted line profile is dominated by the macroscopic velocity of the expanding shock wave of the SN. We are therefore able to trace the evolution of the shock velocity in the dense and partially opaque circumstellar medium (CSM), from ∼ 4800 km s −1 at +48 d, decreasing as t −0.23 to ∼ 2700 km s −1 after a year. We performed spectral modeling of both the broad-and intermediate-velocity components of the Hα line profile. The high-velocity component is consistent with emission from a radially thin, spherical shell located behind the expanding shock with emission wings broadened by electron scattering. We propose that the intermediate component originates from preionized gas from the unshocked dense CSM with the same velocity as the narrow component, ∼ 100 km s −1 , but also that it is broadened by electron scattering. These features provide direct information about the shock structure, which is consistent with model calculations. The spectra exhibit broad O i and [O i] lines that emerge at +144 d and broad Ca ii features. The spectral continua and the spectral energy distributions (SEDs) of SN 2013L after +132 d are well reproduced by a two-component black-body (BB) model; one component represents emitting material with a temperature between 5×10 3 to 1.5×10 4 K (hot component) and the second component is characterized by a temperature around 1-1.5×10 3 K (warm component). The warm component dominates the emission at very late epochs ( +400 d), as is evident from both the last near infrared (NIR) spectrum and MIR observations obtained with the Spitzer Space Telescope. Using the BB fit to the SEDs, we constructed a bolometric light curve that was modeled together with the unshocked CSM velocity and the shock velocity derived from the Hα line modeling. The circumstellar-interaction model of the bolometric light curve reveals a mass-loss rate history with large values ( 1.7 × 10 −2 − 0.15 M yr −1 ) over the ∼25 -40 years before explosion, depending on the radiative efficiency and anisotropies in the CSM. The drop in the light curve at ∼ 350 days and the presence of electron scattering wings at late epochs indicate an anisotropic CSM. The mass-loss rate values and the unshocked-CSM velocity are consistent with the characteristics of a massive star, such as a luminous blue variable (LBV) undergoing strong eruptions, similar to η Carina. Our analysis also suggests a scenario where pre-existing dust grains have a dis...

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Section: Seds and Constructing The Bolometric Light Curvementioning

confidence: 93%

Section: Modeling Of the Spectral Linesmentioning

confidence: 99%

The Carnegie Supernova Project II

Taddia

Stritzinger

Fransson

et al. 2020

A&A

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“…7 is the sizeable peak blueshift of the Hα line. This originates from an optical depth effect (Dessart & Hillier 2005) and is a generic property of SN spectra (Anderson et al 2014), even present in Type IIn SNe (Zhang et al 2012;Dessart et al 2015a). This effect is predicted in spherically symmetric ejecta -asphericity is not necessary.…”

Section: Spectroscopymentioning

confidence: 99%

Supernovae from massive stars with extended tenuous envelopes

Yoon

Livne

Waldman

2018

A&A

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Massive stars with a core-halo structure are interesting objects for stellar physics and hydrodynamics. Using simulations for stellar evolution, radiation hydrodynamics, and radiative transfer, we study the explosion of stars with an extended and tenuous envelope (i.e., stars in which 95% of the mass is contained within 10% of the surface radius or less). We consider both H-rich supergiant and He-giant progenitors resulting from close-binary evolution and dying with a final mass of 2.8-5 M . An extended envelope causes the supernova (SN) shock to brake and a reverse shock to form, sweeping core material into a dense shell. The shock deposited energy, which suffers little degradation from expansion, is trapped in ejecta layers of moderate optical depth, thereby enhancing the SN luminosity at early times. With the delayed 56 Ni heating, we find that the resulting optical and near-IR light curves all exhibit a double-peak morphology. We show how an extended progenitor can explain the blue and featureless optical spectra of some Type IIb and Ib SNe. The dense shell formed by the reverse shock leads to line profiles with a smaller and near-constant width. This ejecta property can explain the statistically narrower profiles of Type IIb compared to Type Ib SNe, as well as the peculiar Hα profile seen in SN 1993J. At early times, our He-giant star explosion model shows a high luminosity, a blue colour, and featureless spectra reminiscent of the Type Ib SN 2008D, suggesting a low-mass progenitor.

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“…Nevertheless, calculating the radiative properties and spectral line emission from the dense shells bounded by a forward and a reverse shock following CSM interaction is a challenge for conventional spectral synthesis and radiation transfer codes (Dessart et al 2015(Dessart et al , 2016. This is due to a variety of reasons.…”

Section: The Origin Of Asassn-15lhmentioning

confidence: 99%

“…The extraordinary luminosities of SLSNe can, in principle, be provided by three different power-input mechanisms: the radioactive decay of large quantities of newly synthesized 56 Ni (M Ni > 10 M e ) in the context of pair-instability supernovae (PISNe; Heger & Woosley 2002;Nomoto et al 2007;Kasen et al 2011;Dessart et al 2013;Kozyreva et al 2014aKozyreva et al , 2014bChatzopoulos et al 2015;Kozyreva & Blinnikov 2015), energy injection by a rapidly spinning newly born magnetar (Ostriker et al 1972;Shklovskii 1976;Kasen & Bildsten 2010;Woosley 2010;Dessart et al 2012;Inserra et al 2013;Metzger et al 2015;Nicholl et al 2015Nicholl et al , 2016Sukhbold & Woosley 2016), and shock heating due to the interaction of SN ejecta with a dense CSM shell (Grasberg & Nadezhin 1986;Chevalier & Fransson 1994;Woosley et al 2007;Chatzopoulos et al 2011Chatzopoulos et al , 2013bChatzopoulos & Wheeler 2012b;Moriya & Tominaga 2012;Moriya et al 2013;Dessart et al 2015;see also Smith & McCray 2007and subsequent discussion in Moriya et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Extreme Supernova Models for the Super-Luminous Transient Asassn-15lh

Chatzopoulos

Wheeler

Vinkó

et al. 2016

ApJ

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The recent discovery of the unprecedentedly super-luminous transient ASASSN-15lh (or SN 2015L) with its UVbright secondary peak challenges all the power-input models that have been proposed for super-luminous supernovae. Here we examine some of the few viable interpretations of ASASSN-15lh in the context of a stellar explosion, involving combinations of one or more power inputs. We model the lightcurve of ASASSN-15lh with a hybrid model that includes contributions from magnetar spin-down energy and hydrogen-poor circumstellar interaction. We also investigate models of pure circumstellar interaction with a massive hydrogen-deficient shell and discuss the lack of interaction features in the observed spectra. We find that, as a supernova, ASASSN-15lh can be best modeled by the energetic core-collapse of an ∼40M e star interacting with a hydrogen-poor shell of ∼20M e . The circumstellar shell and progenitor mass are consistent with a rapidly rotating pulsational pairinstability supernova progenitor as required for strong interaction following the final supernova explosion. Additional energy injection by a magnetar with aninitial period of 1-2 ms and magnetic field of 0.1-1×10 14 G may supply the excess luminosity required to overcome the deficit in single-component models, but this requires more fine-tuning and extreme parameters for the magnetar, as well as the assumption of efficient conversion of magnetar energy into radiation. We thus favor a single-input model where the reverse shock formed in a strong SN ejecta-circumstellar matter interaction following a very powerful core-collapse SN explosion can supply the luminosity needed to reproduce the late-time UV-bright plateau.

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Numerical simulations of superluminous supernovae of type IIn

Cited by 116 publications

References 57 publications

The Carnegie Supernova Project II

The Carnegie Supernova Project II

Supernovae from massive stars with extended tenuous envelopes

Extreme Supernova Models for the Super-Luminous Transient Asassn-15lh

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