Three-dimensional Explosion Geometry of Stripped-envelope Core-collapse Supernovae. II. Modeling of Polarization

Tanaka, Masaomi; Maeda, Keiichi; Mazzali, P. A.; Kawabata, Koji S.; Nomoto, Ken’ichi

doi:10.3847/1538-4357/aa6035

Cited by 33 publications

(29 citation statements)

References 137 publications

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“…Support to the notion that jets play a role in the explosion of many CCSNe comes from observations (e.g., Lopez et al 2014;González-Casanova et al 2014;Milisavljevic et al 2015;Tanaka et al 2017) and theoretical arguments, including numerical simulations (e.g. Bromberg & Tchekhovskoy 2016;Gilkis 2017;Nishimura et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The imprints of the last jets in core collapse supernovae

Bear

Grichener²,

Soker

2017

Monthly Notices of the Royal Astronomical Society

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We analyze the morphologies of three core collapse supernova remnants (CCSNRs) and the energy of jets in other CCSNRs and in Super Luminous Supernovae (SLSNe) of type Ib/Ic/IIb, and conclude that these properties are well explained by the last jets' episode as expected in the jet feedback explosion mechanism of core collapse supernovae (CCSNe). The presence of two opposite protrusions, termed ears, and our comparison of the CCSNR morphologies with morphologies of planetary nebulae strengthen the claim that jets play a major role in the explosion mechanism of CCSNe. We crudely estimate the energy that was required to inflate the ears in two CCSNRs, and assume that the ears were inflated by jets. We find that the energies of the jets that inflated ears in 11 CCSNRs span a range that is similar to that of jets in some energetic CCSNe (SLSNe), and that this energy, only of the last jets' episode, is much less than the explosion energy. This finding is compatible with the jet feedback explosion mechanism of CCSNe, where only the last jets, that carry a small fraction of the total energy carried by earlier jets, are expected to influence the outer parts of the ejecta. We reiterate our call for a paradigm shift from neutrino-driven to jet-driven explosion models of CCSNe.

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Section: Introductionmentioning

confidence: 99%

The imprints of the last jets in core collapse supernovae

Bear

Grichener²,

Soker

2017

Monthly Notices of the Royal Astronomical Society

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“…So at present, signatures of jets cannot break the tie between the two scenarios. Tanaka et al (2017) suggest from their modelling of line polarization of CCSNe that ". .…”

Section: Observational Consequencesmentioning

confidence: 99%

The two promising scenarios to explode core collapse supernovae

Soker

2017

Res. Astron. Astrophys.

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I compare to each other what I consider to be the two most promising scenarios to explode core-collapse supernovae (CCSNe). Both are based on the negative jet feedback mechanism (JFM). In the jittering jets scenario a collapsing core of a single slowly-rotating star can launch jets. The accretion disk or belt (a sub-Keplerian accretion flow concentrated toward the equatorial plane) that launches the jets is intermittent with varying directions of the axis. Instabilities, such as the standing accretion shock instability (SASI), lead to stochastic angular momentum variations that allow the formation of the intermittent accretion disk/belt. According to this scenario no failed CCSNe exist. According to the fixed axis scenario, the core of the progenitor star must be spun up during its late evolutionary phases, and hence all CCSNe are descendants of strongly interacting binary systems, most likely through a common envelope evolution (whether the companion survives or not). Due to the strong binary interaction, the axis of the accretion disk that is formed around the newly born neutron star has a more or less fixed direction. According to the fixed axis scenario, accretion disk/belt are not formed around the newly born neutron star of single stars; they rather end in failed CCSNe. I also raise the possibility that the jittering jets scenario operates for progenitors with initial mass of 8M ⊙ M ZAMS 18M ⊙ , while the fixed axis scenario operates for M ZAMS 18M ⊙ . For the first time these two scenarios are compared to each other, as well as to some aspects of neutrino-driven explosion mechanism. These new comparisons further suggest that the JFM plays a major role in exploding massive stars.

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“…In addition to the continuum polarization, the polarization features across the absorption lines are of interest as they can be a probe of the elemental distribution (e.g., Kasen et al 2003;Tanaka et al 2017). In fact, our data show some changes in the polarization at the wavelengths of some absorption lines.…”

Section: Polarization At the Late Phasementioning

confidence: 79%

Late-phase Spectropolarimetric Observations of Superluminous Supernova SN 2017egm to Probe the Geometry of the Inner Ejecta

Saito

Tanaka

Moriya

et al. 2020

ApJ

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We present our spectropolarimetric observations of SN 2017egm, a Type I superluminous supernova (SLSN-I) in a nearby galaxy NGC 3191, with the Subaru telescope at +185.0 days after the g-band maximum light. This is the first spectropolarimetric observation for SLSNe at late phases. We find that the degree of the polarization in the late phase significantly changes from that measured at the earlier phase. The spectrum at the late phase shows a strong Ca emission line and therefore we reliably estimate the interstellar polarization (ISP) component assuming that the emission line is intrinsically unpolarized. By subtracting the estimated ISP, we find that the intrinsic polarization at the early phase is only ∼0.2%, which indicates an almost spherical photosphere, with an axial ratio ∼1.05. The intrinsic polarization at the late phase increases to ∼0.8%, which corresponds to the photosphere with an axial ratio ∼1.2. A nearly constant position angle of the polarization suggests the inner ejecta are almost axisymmetric. By these observations, we conclude that the inner ejecta are more aspherical than the outer ejecta. This may suggest the presence of a central energy source producing aspherical inner ejecta.

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Three-dimensional Explosion Geometry of Stripped-envelope Core-collapse Supernovae. II. Modeling of Polarization

Cited by 33 publications

References 137 publications

The imprints of the last jets in core collapse supernovae

The imprints of the last jets in core collapse supernovae

The two promising scenarios to explode core collapse supernovae

Late-phase Spectropolarimetric Observations of Superluminous Supernova SN 2017egm to Probe the Geometry of the Inner Ejecta

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