Peculiar Supernovae

Milisavljevic, Dan; Margutti, R.

doi:10.1007/978-94-024-1581-0_8

Cited by 4 publications

(4 citation statements)

References 133 publications

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“…Observations of polarization in some core collapse supernovae (CCSNe) and morphological features of some supernova remnants strongly suggest that jets play a significant role in many, and possibly in most, CCSNe (e.g., Wang et al 2001;Maund et al 2007;Lopez et al 2011;Milisavljevic et al 2013;González-Casanova et al 2014;Margutti et al 2014;Inserra et al 2016;Mauerhan et al 2017;Bear et al 2017;García et al 2017;Lopez & Fesen 2018). Bose et al (2019), as a recent example, study the Type II-P CCSN ASASSN-16at (SN 2016X) and argue that the nebularphase Balmer emission suggests that the 56 Ni in this CCSN has a bipolar morphology.…”

Section: Introductionmentioning

confidence: 99%

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

Kaplan

Soker

2020

Monthly Notices of the Royal Astronomical Society

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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 core collapse supernovae (CCSNe) when the jets interact with the CCSN ejecta. We assume that the central object accretes fall back 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. In our toy model late jets form stronger emission peaks than early jets. Late jets with a kinetic energy of only about one percent 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 one percent of the CCSN energy, and the shocked ejecta mass to be about one percent of the ejecta mass.

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Section: Introductionmentioning

confidence: 99%

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

Kaplan

Soker

2020

Monthly Notices of the Royal Astronomical Society

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“…Many studies have found indications, like polarization in some CCSNe and the morphology of some supernova remnants, for some roles that jets play in possibly most CCSNe (e.g., Wang et al 2001;Maund et al 2007;Smith et al 2012;Lopez et al 2011;Milisavljevic et al 2013;González-Casanova et al 2014;Margutti et al 2014;Inserra et al 2016;Mauerhan et al 2017;Bear et al 2017;García et al 2017;Lopez & Fesen 2018). As well, there are many studies of jetdriven CCSNe that do not consider jittering, and hence are aiming at rare cases, e.g., of progenitors having a very rapidly rotating pre-collapse core (e.g., Khokhlov et al 1999;Aloy et al 2000;Höflich et al 2001;Mac-Fadyen et al 2001;Obergaulinger et al 2006;Burrows et al 2007;Nagakura et al 2011;Takiwaki & Kotake 2011;Lazzati et al 2012;Maeda et al 2012;López-Cámara et al 2013;Mösta et al 2014;Ito et al 2015;Bromberg & Tchekhovskoy 2016;López-Cámara et al 2016;Nishimura et al 2017;Feng et al 2018;Gilkis 2018;Obergaulinger et al 2018).…”

Section: Introductionmentioning

confidence: 99%

Amplifying magnetic fields of a newly born neutron star by stochastic angular momentum accretion in core collapse supernovae

Soker

2020

Res. Astron. Astrophys.

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I present a novel mechanism to boost magnetic field amplification of newly born neutron stars in core collapse supernovae. In this mechanism, that operates in the jittering jets explosion mechanism and comes on top of the regular magnetic field amplification by turbulence, the accretion of stochastic angular momentum in core collapse supernovae forms a neutron star with strong initial magnetic fields but with a slow rotation. The varying angular momentum of the accreted gas, which is unique to the jittering jets explosion mechanism, exerts a varying azimuthal shear on the magnetic fields of the accreted mass near the surface of the neutron star. This, I argue, can form an amplifying effect which I term the stochastic omega (Sω) effect. In the common αω dynamo the rotation has constant direction and value, and hence supplies a constant azimuthal shear, while the convection has a stochastic behavior. In the Sω dynamo the stochastic angular momentum is different from turbulence in that it operates on a large scale, and it is different from a regular rotational shear in being stochastic. The basic assumption is that because of the varying direction of the angular momentum axis from one accretion episode to the next, the rotational flow of an accretion episode stretches the magnetic fields that were amplified in the previous episode. I estimate the amplification factor of the Sω dynamo alone to be ≈ 10. I speculate that the Sω effect accounts for a recent finding that many neutron stars are born with strong magnetic fields.

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“…Jets that drive CCSNe form bipolar morphological features (e.g., Orlando et al 2016;Bear, & Soker 2018), and therefore might account for this 56 Ni morphology. Other observations include the detection of polarisation and the presence of two protruding small lobes on opposite sides of some CCSN remnants (termed 'Ears') (e.g., Wang et al 2001;Maund et al 2007;Milisavljevic et al 2013;González-Casanova et al 2014;Margutti et al 2014;Inserra et al 2016;Mauerhan et al 2017;Bear et al 2017;García et al 2017;Lopez & Fesen 2018). The degree to which jets play roles in the explosion mechanism and in the evolution of CCSNe is still an open question.…”

Section: Introductionmentioning

confidence: 99%

Simulating the inflation of bubbles by late jets in core collapse supernova ejecta

Akashi,

Soker

2020

Preprint

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We conducted three-dimensional hydrodynamical simulations to study the interaction of two late opposite jets with the ejecta of a core collapse supernova (CCSN), and study the bipolar structure that results from this interaction as the jets inflate hot-low-density bubbles. The newly born central object, a neutron star (NS; or a black hole), launches these jets at about 50 to 100 days after explosion. The bubbles cross the photosphere in the polar directions at much earlier times than the regions at the same radii near the equatorial plane. The hot bubbles releases more radiation and the photosphere recedes more rapidly in the tenuous bubble. Our results strengthen earlier claims that were based on toy models that such an interaction might lead to a late peak in the light curve, and that an equatorial observer might see a rapid drop in the light curve. Our results have implications to much earlier jets that explode the star, either jets that the newly born NS launches in a CCSN, or jets that a NS companion that merges with the core of a massive star launches in a common envelope jets supernova (CEJSN) event. Our results add indirect support to the CEJSN scenario for fast blue optical transients, e.g.,

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Peculiar Supernovae

Cited by 4 publications

References 133 publications

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

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

Amplifying magnetic fields of a newly born neutron star by stochastic angular momentum accretion in core collapse supernovae

Simulating the inflation of bubbles by late jets in core collapse supernova ejecta

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