Unusual Supernovae and Alternative Power Sources

Kasen, Daniel

doi:10.1007/978-3-319-20794-0_32-1

Cited by 2 publications

(1 citation statement)

References 60 publications

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“…Given the enormous effort that has gone into explaining normal SN Ia, it is astounding to think that we may have a better understanding of their peculiar cousins, SN Iax. The Extremes of Thermonuclear Supernovae (Taubenberger 2016) Type Ia Supernovae (Maguire 2016) Unusual Supernovae and Alternative Power Sources (Kasen 2017)…”

Section: Discussionmentioning

confidence: 99%

Handbook of Supernovae

Alsabti¹

2016

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Type Iax supernovae (SN Iax), also called SN 2002cx-like supernovae, are the largest class of "peculiar" white dwarf (thermonuclear) supernovae, with over fifty members known. SN Iax have lower ejecta velocity and lower luminosities, and these parameters span a much wider range, than normal type Ia supernovae (SN Ia). SN Iax are spectroscopically similar to some SN Ia near maximum light, but are unique among all supernovae in their late-time spectra, which never become fully "nebular". SN Iax overwhelmingly occur in late-type host galaxies, implying a relatively young population. The SN Iax 2012Z is the only white dwarf supernova for which a pre-explosion progenitor system has been detected. A variety of models have been proposed, but one leading scenario has emerged: a type Iax supernova may be a pure-deflagration explosion of a carbon-oxygen (or hybrid carbon-oxygen-neon) white dwarf, triggered by helium accretion to the Chandrasekhar mass, that does not necessarily fully disrupt the star.

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Section: Discussionmentioning

confidence: 99%

Handbook of Supernovae

Alsabti¹

2016

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SN 2020qlb: A hydrogen-poor superluminous supernova with well-characterized light curve undulations

West

Lunnan

Omand

et al. 2023

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Context. SN 2020qlb (ZTF20abobpcb) is a hydrogen-poor superluminous supernova (SLSN-I) that is among the most luminous (maximum M g = −22.25 mag) and that has one of the longest rise times (77 days from explosion to maximum). We estimate the total radiated energy to be > 2.1 × 10 51 erg. SN 2020qlb has a well-sampled light curve that exhibits clear near and post peak undulations, a phenomenon seen in other SLSNe, whose physical origin is still unknown. Aims. We discuss the potential power source of this immense explosion as well as the mechanisms behind its observed light curve undulations. Methods. We analyze photospheric spectra and compare them to other SLSNe-I. We construct the bolometric light curve using photometry from a large data set of observations from the Zwicky Transient Facility (ZTF), Liverpool Telescope (LT) and Neil Gehrels Swift Observatory and compare it with radioactive, circumstellar interaction and magnetar models. Model residuals and light curve polynomial fit residuals are analyzed to estimate the undulation timescale and amplitude. We also determine host galaxy properties based on imaging and spectroscopy data, including a detection of the [O III]λ4363, auroral line, allowing for a direct metallicity measurement. Results. We rule out the Arnett 56 Ni decay model for SN 2020qlb's light curve due to unphysical parameter results. Our most favored power source is the magnetic dipole spin-down energy deposition of a magnetar. Two to three near peak oscillations, intriguingly similar to those of SN 2015bn, were found in the magnetar model residuals with a timescale of 32 ± 6 days and an amplitude of 6% of peak luminosity. We rule out centrally located undulation sources due to timescale considerations; and we favor the result of ejecta interactions with circumstellar material (CSM) density fluctuations as the source of the undulations.

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Unusual Supernovae and Alternative Power Sources

Cited by 2 publications

References 60 publications

Handbook of Supernovae

Handbook of Supernovae

SN 2020qlb: A hydrogen-poor superluminous supernova with well-characterized light curve undulations

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