TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION

Zhang, Tianmeng; Wang, Xiaofeng; Wu, Chao; Chen, Jun-Cheng; Chen, Jia; Liu, Qin; Huang, Fang; Liang, Jide; Zhao, Xulin; Lin, Lin; Wang, Min; Dennefeld, M.; Zhang, Jujia; Zhai, M.; Wu, Hong; Zhou, Fan; Zou, Hu; Zhou, Xu; Ma, Jun

doi:10.1088/0004-6256/144/5/131

Cited by 104 publications

(41 citation statements)

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“…In our reference model, we find that the bulk of Hα photons arise from regions with an electron scattering optical depth of a few, giving rise to emission in line wings extending to ∼ 3000 km s −1 from line centre, and characterised by a profile with a FWHM of ∼1500 km s −1 . This is somewhat similar to values in SN 2010jl (Zhang et al 2012) at early epochs. However at later times the profiles in SN 2010jl are broader and blue shifted.…”

Section: Spectral Evolutionsupporting

confidence: 86%

“…Two good examples of such SNe IIn are SN 2006gy ) and more recently SN 2010jl (Stoll et al 2011). The latter has extensive photometric and spectroscopic observations (Stoll et al 2011;Zhang et al 2012;Ofek et al 2014;Fransson et al 2014) and also has spectropolarimetric data (Patat et al 2011;Williams et al 2014). How stars produce the outer shell is unclear -it may be material ejected by the pair-production instability (Barkat et al 1967;Woosley et al 2007) or it may be material ejected via a superEddington wind (Owocki et al 2004).…”

Section: Introductionmentioning

confidence: 99%

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Numerical simulations of superluminous supernovae of type IIn

Dessart¹,

Audit²,

Hillier³

2015

Monthly Notices of the Royal Astronomical Society

123

172

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We present numerical simulations that include 1-D Eulerian multi-group radiationhydrodynamics, 1-D non-Local-Thermodynamic-Equilibrium (non-LTE) radiative transfer, and 2-D polarised radiative transfer for super-luminous interacting supernovae (SNe). Our reference model is a ∼10 M ⊙ inner shell with 10 51 erg ramming into a ∼3 M ⊙ cold outer shell (the circumstellar-medium, or CSM) that extends from 10 15 to 2×10 16 cm and moves at 100 km s −1 . We discuss the light curve evolution, which cannot be captured adequately with a grey approach. In these interactions, the shock-crossing time through the optically-thick CSM is much longer than the photon diffusion time. Radiation is thus continuously leaking from the shock through the CSM, in disagreement with the shell-shocked model that is often invoked. Our spectra redden with time, with a peak distribution in the near-UV during the first month gradually shifting to the optical range over the following year. Initially Balmer lines exhibit a narrow line core and the broad line wings that are characteristic of electron scattering in the SNe IIn atmospheres (CSM). At later times they also exhibit a broad blue shifted component which arises from the cold dense shell. Our model results are broadly consistent with the bolometric light curve and spectral evolution observed for SN 2010jl. Invoking a prolate pole-to-equator density ratio in the CSM, we can also reproduce the ∼2% continuum polarisation, and line depolarisation, observed in SN 2010jl. By varying the inner shell kinetic energy and the mass and extent of the outer shell, a large range of peak luminosities and durations, broadly compatible with super-luminous SNe IIn like 2010jl or 2006gy, can be produced.

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Section: Spectral Evolutionsupporting

confidence: 86%

Section: Introductionmentioning

confidence: 99%

Numerical simulations of superluminous supernovae of type IIn

Dessart¹,

Audit²,

Hillier³

2015

Monthly Notices of the Royal Astronomical Society

123

172

View full text Add to dashboard Cite

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“…They constitute a non-negligible fraction of CC-SNe (∼ 7%, e.g., Li et al 2011;Smith et al 2011;Shivvers et al 2017). The well-studied examples include SN 1988Z (Stathakis & Sadler 1991;Turatto et al 1993;van Dyk et al 1993;Chugai & Danziger 1994;Aretxaga et al 1999), 1998S (Fassia et al 2000(Fassia et al , 2001Leonard et al 2000), and 2010jl (Patat et al 2011;Stoll et al 2011;Zhang et al 2012;Fransson et al 2014;Ofek et al 2014a). The ejecta-CSM collision can efficiently dissipate the kinetic energy of the ejecta and release the dissipated energy as bright thermal radiation.…”

Section: Introductionmentioning

confidence: 99%

Supernova Ejecta Interacting with a Circumstellar Disk. I. Two-dimensional Radiation-hydrodynamic Simulations

Suzuki

Moriya

Takiwaki

2019

ApJ

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We perform a series of two-dimensional radiation-hydrodynamic simulations of the collision between supernova ejecta and circumstellar media (CSM). The hydrodynamic interaction of a fast flow and the surrounding media efficiently dissipates the kinetic energy of the fast flow and considered as a dominant energy source for a specific class of core-collapse supernovae. Despite some observational evidence for aspherical ejecta and/or CSM structure, multi-dimensional effects in the ejecta-CSM interaction are relatively unexplored. Our numerical simulations equipped with an adaptive mesh refinement technique successfully reproduce hydrodynamic instabilities developing around the ejecta-CSM interface. We also investigate effects of disk-like CSM on the dynamical evolution of supernova ejecta and bolometric light curves. We find that emission powered by ejecta-disk interaction exhibits significant viewing angle dependence. For a line of sight close to the symmetry axis, the observer directly sees the supernova ejecta, leading to a short brightening timescale. For an observer seeing the emission through the CSM disk, thermal photons diffuse throughout the CSM and thus the light curve is severely smeared out.

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“…The He i 5876, 7065 Å features are stronger in SN 2017hcc and SN 2010jl than in SN 2012ab. An unblended signature of a Na i D feature was found in SN 2012ab (Bilinski et al 2018) which is negligible in SN 2017hcc and SN 2010jl (Zhang et al 2012) indicating negligible reddening (see Section 3.1) along the line of sight caused by the host galaxies.…”

Section: Light Curves and Spectral Featuresmentioning

confidence: 99%

“…Comparison of SN 2017hcc, SN 2012ab(Gangopadhyay et al 2019) and SN 2010jl(Zhang et al 2012) spectra at similar epochs. Prominent Balmer and He i lines are also marked.…”

mentioning

confidence: 99%

On the observational behaviour of the highly polarized Type IIn supernova SN 2017hcc

Kumar

Eswaraiah

Singh

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present the results based on photometric (Swift UVOT), broad-band polarimetric (V and R-band) and optical spectroscopic observations of the Type IIn supernova (SN) 2017hcc. Our study is supplemented with spectropolarimetric data available in literature for this event. The post-peak light curve evolution is slow (∼ 0.2 mag 100 d −1 in b-band). The spectrum of ∼ +27 d shows a blue continuum with narrow emission lines, typical of a Type IIn SN. Archival polarization data along with the Gaia DR2 distances have been utilized to evaluate the interstellar polarization (ISP) towards the SN direction which is found to be P IS P = 0.17 ± 0.02 per cent and θ IS P = 140 • ± 3 • . To extract the intrinsic polarization of SN 2017hcc, both the observed and the literature polarization measurements were corrected for ISP. We noticed a significant decline of ∼ 3.5 per cent (V-band) in the intrinsic level of polarization spanning a period of ∼ 2 months. In contrast, the intrinsic polarization angles remain nearly constant at all epochs. Our study indicates a substantial variation in the degree of asymmetry in either the ejecta and/or the surrounding medium of SN 2017hcc. We also estimate a mass-loss rate oḟ M = 0.12 M yr −1 (for v w = 20 km s −1 ) which suggests that the progenitor of SN 2017hcc is most likely a Luminous Blue Variable.

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TYPE IIn SUPERNOVA SN 2010jl: OPTICAL OBSERVATIONS FOR OVER 500 DAYS AFTER EXPLOSION

Cited by 104 publications

References 50 publications

Numerical simulations of superluminous supernovae of type IIn

Numerical simulations of superluminous supernovae of type IIn

Supernova Ejecta Interacting with a Circumstellar Disk. I. Two-dimensional Radiation-hydrodynamic Simulations

On the observational behaviour of the highly polarized Type IIn supernova SN 2017hcc

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