Modeling Light Curves of Bipolar Core Collapse Supernovae from the Equatorial Plane

Soker, Noam; Kaplan, Noa

doi:10.3847/1538-4357/abcd9d

Cited by 5 publications

(2 citation statements)

References 60 publications

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“…The 56 Ni masses derived from the two models are larger than the upper limit (∼0.2 M e ) of the 56 Ni mass that can be synthesized by the neutrino-power mechanism (Sukhbold et al 2016;Ertl et al 2020). Soker & Kaplan (2021) fit the V-band data of SN 2018gk using a two-component bipolar model. The photometry in all other bands has not been used.…”

Section: Introductionmentioning

confidence: 99%

SN 2018gk Revisited: the Photosphere, the Central Engine, and the Putative Dust

Wang

Gan

et al. 2023

ApJ

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We perform a comprehensive study of the physical properties of SN 2018gk, which is a luminous Type IIb supernova (SN). We find that the early-time photospheric velocity varies from a larger value to a smaller one before the photosphere reaches a temperature floor. We generalize the photosphere modulus and fit the multiband light curves (LCs) of SN 2018gk. We find that the 56Ni mass model requires ∼0.90 M ⊙ of 56Ni, which is larger than the derived ejecta mass (∼0.10 M ⊙). Alternatively, we use the magnetar plus 56Ni and the fallback plus 56Ni models to fit the LCs of SN 2018gk, finding that the two models can fit the LCs. We favor the magnetar plus 56Ni model since the parameters are rather reasonable (M ej = 1.65 M ⊙, M Ni = 0.05 M ⊙, which is smaller than the upper limit of the 56Ni mass that can by synthesized by neutrino-powered core-collapse SNe, B = 6.52 × 1014 G, which is comparable to magnetic fields in luminous and superluminous SNe studied in the literature, and P 0 = 10.42 ms, which is comparable to initial periods for luminous SNe), while the validity of the fallback plus 56Ni model depends on the accretion efficiency (η). Therefore, we suggest that SN 2018gk might be an SN IIb powered mainly by a central engine. Finally, we confirm the near-IR excesses of the spectral energy distributions of SN 2018gk at some epochs and constrain the physical properties of the putative dust using the blackbody plus dust emission model.

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Section: Introductionmentioning

confidence: 99%

SN 2018gk Revisited: the Photosphere, the Central Engine, and the Putative Dust

Wang

Gan

et al. 2023

ApJ

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“…This evolution takes place in an ISM with a uniform magnetic field, producing an asymmetric circumstellar medium in which the SN ejecta expands, and results in a projected rectangular morphology. Other studies on (a)symmetric core-collapse SNRs include Meyer et al (2015Meyer et al ( , 2020Meyer et al ( , 2021a, Orlando et al (2021Orlando et al ( , 2022, Soker (2021), andKaplan (2021).…”

Section: Introductionmentioning

confidence: 99%

The sculpting of rectangular and jet-like morphologies in supernova remnants by anisotropic equatorially confined progenitor stellar winds

Velázquez

Meyer

Chiotellis

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Thermonuclear and core-collapse supernova remnants (SNRs) are the nebular leftovers of defunct stars. Their morphology and emission properties provide insights into the evolutionary history of the progenitor star. But while some SNRs are spherical, as expected from a point-like explosion expanding into a roughly uniform medium, many others exhibit complex non-spherical morphologies which are often not easily explained. In this work, we use three-dimensional magnetohydrodynamic simulations to show that rectangular and jet-like morphologies can be explained by supernovae (SNe), either type Ia or type II, expanding within anisotropic, bipolar stellar wind bubbles driven by the progenitor star. The stellar wind has an anisotropic density distribution, which channels the SN ejecta differently depending on the anisotropy characteristics. We compute synthetic thermal (X-ray) and non-thermal (synchrotron) emission maps from our numerical simulations to compare with observations. We find rectangular morphologies are generated when the stellar wind has a high mass loss rate and forms a dense, narrow disk at the equatorial region. Instead, a jet-like or ear-like morphology is obtained when the stellar wind develops a wide, dense disk. Stellar winds with low mass-loss rates do not strongly influence the SNR morphology. Finally, our synthetic synchrotron and X-ray maps for the high mass-loss rate case qualitatively agree with the observations of the SNRs G332.5-5.6 and G290.1-0.8.

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Supernova remnants of red supergiants: From barrels to loops

Meyer,

Velázquez,

Pohl

et al. 2024

A&A

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Core-collapse (CC) supernova remnants (SNRs) are the nebular leftovers of defunct massive stars that died during a supernova explosion, mostly while undergoing the red supergiant phase of their evolution. The morphology and emission properties of those remnants are a function of the distribution of circumstellar material at the moment of the supernova, as well as the intrinsic properties of the explosion and those of the ambient medium. By means of 2.5-dimensional (2.5D) numerical magneto-hydrodynamic (MHD) simulations, we modelled the long-term evolution of SNRs generated by runaway rotating massive stars moving into a magnetised interstellar medium (ISM). Radiative transfer calculations reveal that the projected non-thermal emission of SNRs decreases over time, namely: older remnants are fainter than younger ones. Older ($80\ kyr$) SNRs whose progenitors were moving with a space velocity corresponding to a Mach number of $M=1$ ($v_ km\ $) in the Galactic plane of the interstellar medium ($n_ ISM $) are brighter in synchrotron than when moving with a Mach number of $M=2$ ($v_ km\ $). We show that runaway red supergiant progenitors first induce an asymmetric non-thermal $1.4\ GHz$ barrel-like synchrotron SNRs (at the age of about $8\ kyr$), before further evolving to adopt a Cygnus-loop-like shape (at about $80\ kyr$). It is conjectured that a significative fraction of SNRs are currently in this bilateral-to-Cygnus loop evolutionary sequence. Therefore, this population should be taken into account with repect to interpreting the data as part of the forthcoming Cherenkov Telescope Array (CTA) observatory.

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Modeling Light Curves of Bipolar Core Collapse Supernovae from the Equatorial Plane

Cited by 5 publications

References 60 publications

SN 2018gk Revisited: the Photosphere, the Central Engine, and the Putative Dust

SN 2018gk Revisited: the Photosphere, the Central Engine, and the Putative Dust

The sculpting of rectangular and jet-like morphologies in supernova remnants by anisotropic equatorially confined progenitor stellar winds

Supernova remnants of red supergiants: From barrels to loops

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