scholarly journals Emission peaks in the light curve of core collapse supernovae by late jets

2020 ◽  
Vol 492 (2) ◽  
pp. 3013-3020 ◽  
Author(s):  
Noa Kaplan ◽  
Noam Soker
Keyword(s):  
Black Hole ◽  
Kinetic Energy ◽  
Light Curve ◽  
Emission Peak ◽  
Light Curves ◽  
Core Collapse ◽  
Spherically Symmetric ◽  
Emission Power ◽  
Strong Emission ◽  
Central Object

ABSTRACT We build a toy model where the central object, i.e. a newly born neutron star or a black hole, launches jets at late times and show that these jets might account for peaks in the light curve of some peculiar (i.e. having unusual light curves) core collapse supernovae (CCSNe) when the jets interact with the CCSN ejecta. We assume that the central object accretes fallback material and launches two short-lived opposite jets weeks to months after the explosion. We model each jet-ejecta interaction as a spherically symmetric ‘mini-explosion’ that takes place inside the ejecta. We assume that each ‘mini-explosion’ adds emission that is symmetric in time around the late peak, and with a rise in emission power that has the same slope as that of the main CCSN light curve. In total, we use 12 parameters in the toy model. In our toy model, late jets form stronger emission peaks than early jets. Late jets with a kinetic energy of only about one per cent of the kinetic energy of the CCSN itself might form strong emission peaks. We apply our toy model to the brightest peak of the enigmatic CCSN iPTF14hls that has several extra peaks in its light curve. We can fit this emission peak with our toy model when we take the kinetic energy of the jets to be about 1–2 per cent of the CCSN energy, and the shocked ejecta mass to be about 3 per cent of the ejecta mass.

scholarly journals The Flavours of SN II Light Curves

2011 ◽  
Vol 7 (S279) ◽  
pp. 34-39 ◽  
Author(s):  
Iair Arcavi
Keyword(s):  
Light Curve ◽  
Rare Events ◽  
Light Curves ◽  
Host Galaxy ◽  
Core Collapse ◽  
Type Ii

AbstractWe present R-Band light curves of Type II supernovae (SNe) from the Caltech Core Collapse Program (CCCP). With the exception of interacting (Type IIn) SNe and rare events with long rise times, we find that most light curve shapes belong to one of three distinct classes: plateau, slowly declining and rapidly declining events. The latter class is composed solely of Type IIb SNe which present similar light curve shapes to those of SNe Ib, suggesting, perhaps, similar progenitor channels. We do not find any intermediate light curves, implying that these subclasses are unlikely to reflect variance of continuous parameters, but rather might result from physically distinct progenitor systems, strengthening the suggestion of a binary origin for at least some stripped SNe. We find a large plateau luminosity range for SNe IIP, while the plateau lengths seem rather uniform at approximately 100 days. We present also host galaxy trends from the Palomar Transien Factory (PTF) core collapse SN sample, which augment some of the photometric results.

scholarly journals Radio Observations of SN2004dk with VLITE Confirm Late-time Rebrightening

2021 ◽  
Vol 923 (1) ◽  
pp. 32
Author(s):  
A. Balasubramanian ◽  
A. Corsi ◽  
E. Polisensky ◽  
T. E. Clarke ◽  
N. E. Kassim
Keyword(s):  
Mass Loss ◽  
Strong Interaction ◽  
Light Curves ◽  
Core Collapse ◽  
Late Time ◽  
Spherically Symmetric ◽  
Complex Environment ◽  
Radio Observations ◽  
The Galaxy ◽  
Using Data

Abstract The study of stripped-envelope core-collapse supernovae (SNe), with evidence for strong interaction of SN ejecta with the circumstellar medium (CSM), provides insights into the pre-supernova progenitor, and a fast-forwarded view of the progenitor mass-loss history. In this context, we present late-time radio observations of SN 2004dk, a Type Ibc supernova located in the galaxy NGC 6118, at a distance of d L ≈ 23 Mpc. About 10 yr after explosion, SN 2004dk has shown evidence for Hα emission, possibly linked to the SN ejecta interacting with a H-rich CSM. Using data from the VLA Low Band Ionosphere and Transient Experiment (VLITE), we confirm the presence of a late-time radio rebrightening accompanying the observed Hα emission. We model the SN 2004dk radio light curves within the (spherically symmetric) synchrotron-self-absorption (SSA) model. Within this model, our VLITE observations combined with previously collected VLA data favor an interpretation of SN 2004dk as a strongly CSM-interacting radio SN going through a complex environment shaped by nonsteady mass loss from the SN progenitor.

scholarly journals Jet-shaped geometrically modified light curves of core-collapse supernovae

2020 ◽  
Vol 494 (4) ◽  
pp. 5909-5916
Author(s):  
Noa Kaplan ◽  
Noam Soker
Keyword(s):  
Light Curve ◽  
Optical Depth ◽  
Equatorial Plane ◽  
Effective Temperature ◽  
Light Curves ◽  
Core Collapse ◽  
Low Density ◽  
Radiated Energy ◽  
Spherical Explosion

ABSTRACT We build three simple bipolar ejecta models for core-collapse supernovae (CCSNe), as expected when the explosion is driven by strong jets, and show that for an observer located in the equatorial plane of the ejecta, the light curve has a rapid luminosity decline, and even an abrupt drop. In calculating the geometrically modified photosphere we assume that the ejecta has an axisymmetrical structure composed of an equatorial ejecta and faster polar ejecta, and has a uniform effective temperature. At early times the photosphere in the polar ejecta grows faster than the equatorial one, leading to higher luminosity relative to a spherical explosion. The origin of the extra radiated energy is the jets. At later times the optical depth decreases faster in the polar ejecta, and the polar photosphere becomes hidden behind the equatorial ejecta for an observer in the equatorial plane, leading to a rapid luminosity decline. For a model where the jets inflate two low-density polar bubbles, the luminosity decline might be abrupt. This model enables us to fit the abrupt decline in the light curve of SN 2018don.

scholarly journals Light Curve Modeling of Superluminous Supernovae

2013 ◽  
Vol 9 (S296) ◽  
pp. 86-89
Author(s):  
Takashi Moriya ◽  
Sergei I. Blinnikov ◽  
Nozomu Tominaga ◽  
Naoki Yoshida ◽  
Masaomi Tanaka ◽  
...  
Keyword(s):  
Kinetic Energy ◽  
Light Curve ◽  
Mass Loss ◽  
Numerical Simulations ◽  
Radiation Energy ◽  
Light Curves ◽  
Physical Parameters ◽  
Radiation Hydrodynamics ◽  
One Dimensional ◽  
Curve Modeling

AbstractOrigins of superluminous supernovae (SLSNe) discovered by recent SN surveys are still not known well. One idea to explain the huge luminosity is the collision of dense CSM and SN ejecta. If SN ejecta is surrounded by dense CSM, the kinetic energy of SN ejecta is efficiently converted to radiation energy, making them very bright. To see how well this idea works quantitatively, we performed numerical simulations of collisions of SN ejecta and dense CSM by using one-dimensional radiation hydrodynamics code STELLA and obtained light curves (LCs) resulting from the collision. First, we show the results of our LC modeling of SLSN 2006gy. We find that physical parameters of dense CSM estimated by using the idea of shock breakout in dense CSM (e.g., Chevalier & Irwin 2011, Moriya & Tominaga 2012) can explain the LC properties of SN 2006gy well. The dense CSM's radius is about 1016 cm and its mass about 15 M⊙. It should be ejected within a few decades before the explosion of the progenitor. We also discuss how LCs change with different CSM and SN ejecta properties and origins of the diversity of H-rich SLSNe. This can potentially be a probe to see diversities in mass-loss properties of the progenitors. Finally, we also discuss a possible signature of SN ejecta-CSM interaction which can be found in H-poor SLSN.

scholarly journals Simulated Radio Images and Light Curves of SN 1993J

2005 ◽  
Vol 192 ◽  
pp. 47-52
Author(s):  
Vikram V. Dwarkadas ◽  
Amy J. Mioduszewski ◽  
Lewis T. Ball
Keyword(s):  
High Resolution ◽  
Light Curve ◽  
Numerical Simulations ◽  
Density Profile ◽  
Radiation Transfer ◽  
Light Curves ◽  
Single Frequency ◽  
Spherically Symmetric ◽  
Self Similar ◽  
Best Fit

SummaryWe present calculations of the radio images and light curves from supernovae, based on high-resolution numerical simulations of the hydrodynamics and radiation transfer in a spherically symmetric medium. As a specific example we model the emission from SN1993J. This supernova does not appear to be expanding in a self-similar fashion, and cannot be adequately fitted with the often-used analytic mini-shell model. We present a good fit to the radio evolution at a single frequency. Both free-free absorption and synchrotron self-absorption are needed to fit the light curve at early times, and a circumstellar density profile of ρ ~ r−1.7 provides the best fit to the later data. Comparisons of VLBI images of SN1993J with synthetic model images suggest that internal free-free absorption completely obscures emission at 8.4 GHz passing through the center of the supernova for the first few tens of years after explosion.

scholarly journals Synthetic observables for electron-capture supernovae and low-mass core collapse supernovae

2021 ◽  
Vol 503 (1) ◽  
pp. 797-814
Author(s):  
Alexandra Kozyreva ◽  
Petr Baklanov ◽  
Samuel Jones ◽  
Georg Stockinger ◽  
Hans-Thomas Janka
Keyword(s):  
Radiative Transfer ◽  
Light Curve ◽  
Electron Capture ◽  
Mass Range ◽  
Light Curves ◽  
Initial Mass ◽  
Core Collapse ◽  
Initial Composition ◽  
Solar Metallicity ◽  
Low Mass

ABSTRACT Stars in the mass range from 8 M⊙ to 10 M⊙ are expected to produce one of two types of supernovae (SNe), either electron-capture supernovae (ECSNe) or core-collapse supernovae (CCSNe), depending on their previous evolution. Either of the associated progenitors retain extended and massive hydrogen-rich envelopes and the observables of these SNe are, therefore, expected to be similar. In this study, we explore the differences in these two types of SNe. Specifically, we investigate three different progenitor models: a solar-metallicity ECSN progenitor with an initial mass of 8.8 M⊙, a zero-metallicity progenitor with 9.6 M⊙, and a solar-metallicity progenitor with 9 M⊙, carrying out radiative transfer simulations for these progenitors. We present the resulting light curves for these models. The models exhibit very low photospheric velocity variations of about 2000 km s−1; therefore, this may serve as a convenient indicator of low-mass SNe. The ECSN has very unique light curves in broad-bands, especially the U band, and does not resemble any currently observed SN. This ECSN progenitor being part of a binary will lose its envelope for which reason the light curve becomes short and undetectable. The SN from the 9.6 M⊙ progenitor exhibits also quite an unusual light curve, explained by the absence of metals in the initial composition. The artificially iron-polluted 9.6 M⊙ model demonstrates light curves closer to normal SNe IIP. The SN from the 9 M⊙ progenitor remains the best candidate for so-called low-luminosity SNe IIP like SN 1999br and SN 2005cs.

scholarly journals The rise and fall of an extraordinary Ca-rich transient

2020 ◽  
Vol 635 ◽  
pp. A186 ◽  
Author(s):  
S. J. Prentice ◽  
K. Maguire ◽  
A. Flörs ◽  
S. Taubenberger ◽  
C. Inserra ◽  
...  
Keyword(s):  
Kinetic Energy ◽  
Light Curves ◽  
Emission Lines ◽  
Core Collapse ◽  
Abundance Distribution ◽  
Diverse Range ◽  
Transient Event ◽  
Explosion Mechanism ◽  
Specific Kinetic Energy ◽  
Phase Spectra

This work presents the observations and analysis of ATLAS19dqr/SN 2019bkc, an extraordinary rapidly evolving transient event located in an isolated environment, tens of kiloparsecs from any likely host. Its light curves rise to maximum light in 5−6 d and then display a decline of Δm15 ∼ 5 mag. With such a pronounced decay, it has one of the most rapidly evolving light curves known for a stellar explosion. The early spectra show similarities to normal and “ultra-stripped” type Ic SNe, but the early nebular phase spectra, which were reached just over two weeks after explosion, display prominent calcium lines, marking SN 2019bkc as a Ca-rich transient. The Ca emission lines at this phase show an unprecedented and unexplained blueshift of 10 000–12 000 km s−1. Modelling of the light curve and the early spectra suggests that the transient had a low ejecta mass of 0.2−0.4 M⊙ and a low kinetic energy of (2−4) × 1050 erg, giving a specific kinetic energy Ek/Mej ∼ 1 [1051 erg]/M⊙. The origin of this event cannot be unambiguously defined. While the abundance distribution used to model the spectra marginally favours a progenitor of white dwarf origin through the tentative identification of Ar II, the specific kinetic energy, which is defined by the explosion mechanism, is found to be more similar to an ultra-stripped core-collapse events. SN 2019bkc adds to the diverse range of physical properties shown by Ca-rich events.

scholarly journals Two stripped envelope supernovae with circumstellar interaction

2020 ◽  
Vol 643 ◽  
pp. A79
Author(s):  
J. Sollerman ◽  
C. Fransson ◽  
C. Barbarino ◽  
C. Fremling ◽  
A. Horesh ◽  
...  
Keyword(s):  
Light Curve ◽  
Light Curves ◽  
X Rays ◽  
Strong Emission ◽  
Circumstellar Material ◽  
High Ionization ◽  
New Period ◽  
Rich Material ◽  
Narrow Emission

Context. We present observations of SN 2019tsf (ZTF19ackjszs) and SN 2019oys (ZTF19abucwzt). These two stripped envelope (SE) Type Ib supernovae (SNe) suddenly showed a (re-)brightening in their late light curves. We investigate this in the context of circumstellar material (CSM) interaction with previously ejected material, a phenomenon that is unusual among SE SNe. Aims. We use our follow-up photometry and spectroscopy for these supernovae to demonstrate the presence of CSM interaction, estimate the properties of the CSM, and discuss why the signals are so different for the two objects. Methods. We present and analyze observational data, consisting of optical light curves and spectra. For SN 2019oys, we also have detections in radio as well as limits from UV and X-rays. Results. Both light curves show spectacular re-brightening after about 100 days. In the case of SN 2019tsf, the re-brightening is followed by a new period of decline, and the spectra never show signs of narrow emission lines that would indicate CSM interaction. On the contrary, SN 2019oys made a spectral makeover from a Type Ib to a spectrum clearly dominated by CSM interaction at the light curve brightening phase. Deep Keck spectra reveal a plethora of narrow high-ionization lines, including coronal lines, and the radio observations show strong emission. Conclusions. The rather similar light curve behavior – with a late linear re-brightening – of these two Type Ib SE SNe indicate CSM interaction as the powering source. For SN 2019oys the evidence for a phase where the ejecta hit H-rich material, likely ejected from the progenitor star, is conspicuous. We observe strong narrow lines of H and He, but also a plethora of high-ionization lines, including coronal lines, revealing shock interaction. Spectral simulations of SN 2019oys show two distinct density components, one with density ≳109 cm−3, dominated by somewhat broader, low-ionization lines of H I, He I, Na I, and Ca II, and one with narrow, high-ionization lines at a density ∼106 cm−3. The former is strongly affected by electron scattering, while the latter is unaffected. The evidence for CSM interaction in SN 2019oys is corroborated by detections in radio. On the contrary, for SN 2019tsf, we find little evidence in the spectra for any CSM interaction.

scholarly journals SEARCH FOR GRAVITATIONAL WAVES FROM SUPERNOVAE AND LONG GRBS

2013 ◽  
Vol 53 (A) ◽  
pp. 736-741 ◽  
Author(s):  
Maurice H.P.M. Van Putten
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Strong Interaction ◽  
Light Curves ◽  
Matched Filtering ◽  
Core Collapse ◽  
Local Universe ◽  
Wave Emission ◽  
Density Matter

We report on evidence for black hole spindown in the light curves of the BATSE catalogue of 1491 long GRBs by application of matched filtering. This observation points to a strong interaction of the black hole with surrounding high density matter at the ISCO, inducing non-axisymmetric instabilities sustained by cooling in gravitational wave emission. Opportunities for LIGO-Virgo and the recently funded KAGRA experiments are highlighted, for long GRBs with and without supernovae and for hyper-energetic core-collapse supernovae within a distance of about 35Mpc in the Local Universe.

scholarly journals PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses

2020 ◽  
Vol 497 (3) ◽  
pp. 3542-3556
Author(s):  
E Pian ◽  
P A Mazzali ◽  
T J Moriya ◽  
A Rubin ◽  
A Gal-Yam ◽  
...  
Keyword(s):  
Kinetic Energy ◽  
Light Curve ◽  
Lower Energy ◽  
Rest Frame ◽  
Main Sequence ◽  
Gamma Ray ◽  
Core Collapse ◽  
Curve Shape ◽  
Maximum Brightness ◽  
The Core

ABSTRACT The hydrogen-poor supernova (SN) PTF11rka (z = 0.0744), reported by the Palomar Transient Factory, was observed with various telescopes starting a few days after the estimated explosion time of 2011 December 5 UT and up to 432 rest-frame days thereafter. The rising part of the light curve was monitored only in the RPTF filter band, and maximum in this band was reached ∼30 rest-frame days after the estimated explosion time. The light curve and spectra of PTF11rka are consistent with the core-collapse explosion of a ∼10 M⊙ carbon–oxygen core evolved from a progenitor of main-sequence mass 25–40 M⊙, that liberated a kinetic energy Ek≈4 × 1051 erg, expelled ∼8 M⊙ of ejecta, and synthesized ∼0.5 M⊙ of 56Ni. The photospheric spectra of PTF11rka are characterized by narrow absorption lines that point to suppression of the highest ejecta velocities (≳ 15 000 km s−1). This would be expected if the ejecta impacted a dense, clumpy circumstellar medium. This in turn caused them to lose a fraction of their energy (∼5 × 1050 erg), less than 2 per cent of which was converted into radiation that sustained the light curve before maximum brightness. This is reminiscent of the superluminous SN 2007bi, the light-curve shape and spectra of which are very similar to those of PTF11rka, although the latter is a factor of 10 less luminous and evolves faster in time. PTF11rka is in fact more similar to gamma-ray burst SNe in luminosity, although it has a lower energy and a lower Ek/Mej ratio.

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