TOWARD CONNECTING CORE-COLLAPSE SUPERNOVA THEORY WITH OBSERVATIONS. I. SHOCK REVIVAL IN A 15<i>M</i><sub>☉</sub>BLUE SUPERGIANT PROGENITOR WITH SN 1987A ENERGETICS

Handy, Timothy; Plewa, T.; Odrzywołek, A.

doi:10.1088/0004-637x/783/2/125

Cited by 46 publications

(89 citation statements)

References 53 publications

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“…Lower (higher) energies produce lower (higher) iron velocities and lower (higher) X-ray fluxes at odds with the observations. We note that the explosion energies found are at the upper end of the range of values, E exp = 0.8 − 2.0 × 10 51 erg, proposed in the literature for SN 1987A (see Table 1 in Handy et al 2014). From bolometric lightcurve fitting what can be constrained is not the explosion energy itself but the ratio between the explosion energy, E exp , and the mass of hydrogen envelope, M env (e.g.…”

Section: Early Distribution and Mixing Of Ejecta In The Remnantmentioning

confidence: 72%

Hydrodynamic simulations unravel the progenitor-supernova-remnant connection in SN 1987A

Orlando

Ono

Nagataki

et al. 2020

A&A

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Context. Massive stars end their lives with catastrophic supernova (SN) explosions. Key information on the explosion processes and on the progenitor stars can be extracted from observations of supernova remnants (SNRs), the outcome of SNe. Deciphering these observations however is challenging because of the complex morphology of SNRs. Aims. We aim at linking the dynamical and radiative properties of the remnant of SN 1987A to the geometrical and physical characteristics of the parent aspherical SN explosion and to the internal structure of its progenitor star. Methods. We performed comprehensive three-dimensional hydrodynamic simulations which describe the long-term evolution of SN 1987A from the onset of the SN to the full-fledged remnant at the age of 50 years, accounting for the pre-SN structure of the progenitor star. The simulations include all physical processes relevant for the complex phases of SN evolution and for the interaction of the SNR with the highly inhomogeneous ambient environment around SN 1987A. Furthermore the simulations follow the life cycle of elements from the synthesis in the progenitor star, through the nuclear reaction network of the SN, to the enrichment of the circumstellar medium through mixing of chemically homogeneous layers of ejecta. From the simulations, we synthesize observables to be compared with observations. Results. By comparing the model results with observations, we constrained the initial SN anisotropy causing Doppler shifts observed in emission lines of heavy elements from ejecta, and leading to the remnant evolution observed in the X-ray band in the last thirty years. In particular, we found that the high mixing of ejecta unveiled by high redshifts and broadenings of [Fe II] and 44 Ti lines require a highly asymmetric SN explosion channeling a significant fraction of energy along an axis almost lying in the plane of the central equatorial ring around SN 1987A, roughly along the line-of-sight but with an offset of 40 o , with the lobe propagating away from the observer slightly more energetic than the other. Furthermore, we found unambiguously that the observed distribution of ejecta and the dynamical and radiative properties of the SNR can be best reproduced if the structure of the progenitor star was that of a blue supergiant resulted from the merging of two massive stars.

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Section: Early Distribution and Mixing Of Ejecta In The Remnantmentioning

confidence: 72%

Hydrodynamic simulations unravel the progenitor-supernova-remnant connection in SN 1987A

Orlando

Ono

Nagataki

et al. 2020

A&A

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“…The calibration aims at producing the explosion energy and ejected 56 Ni mass of SN1987A compatible with observations, for which the best values are E exp =(1.50±0.12)×10 51 erg (Utrobin 2005), E exp ∼1.3×10 51 erg (Utrobin & Chugai 2011), and M Ni =0.0723-0.0772 M e (Utrobin et al 2014), but numbers reported by other authors cover a considerable range (see Handy et al 2014 for a compilation). The explosion energy that we accept for an SN1987A model in the calibration process is guided by the ejected 56 Ni mass (which fully accounts for short-time and long-time fallback) and a ratio of E exp to ejecta mass in the ballpark of estimates based on light-curve analyses (see Table 1 for our values).…”

Section: Progenitor Modelsmentioning

confidence: 99%

A Two-Parameter Criterion for Classifying the Explodability of Massive Stars by the Neutrino-Driven Mechanism

Ertl

Janka

Woosley

et al. 2016

ApJ

441

697

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Thus far, judging the fate of a massive star (either a neutron star [NS]or a black hole) solely by its structure prior to core collapse has been ambiguous. Our work and previous attempts find a nonmonotonic variation of successful and failed supernovae with zero-age main-sequence mass, for which no single structural parameter can serve as a good predictive measure. However, we identify two parameters computed from the pre-collapse structure of the progenitor, which in combination allow for a clear separation of exploding and nonexploding cases with only afew exceptions (∼1%-2.5%) in our set of 621 investigated stellar models. One parameter is M 4 , defining the normalized enclosed mass for a dimensionless entropy per nucleon of s=4, and the other is dm M dr 1000 km s, being the normalized massderivative at this location. The two parameters μ 4 and M 4 μ 4 can be directly linked to the mass-infall rate, Ṁ , of the collapsing star and the electron-type neutrino luminosity of the accreting proto-NS, L M M ns eμ n , which play a crucial role in the "critical luminosity" concept for the theoretical description of neutrino-driven explosions as runaway phenomenaof the stalled accretion shock. All models were evolved employing the approach of Uglianoetal. for simulating neutrino-driven explosions in spherical symmetry. The neutrino emission of the accretion layer is approximated by a gray transport solver, while the uncertain neutrino emission of the 1.1 M e proto-NS core is parameterized by an analytic model. The free parameters connected to the core-boundary prescription are calibrated to reproduce the observables of SN1987A for five different progenitor models.

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“…There is obviously justification for varying α turb within reasonable bounds on several grounds: While the underlying scaling law for the turbulent Mach number likely holds in 3D as well, the relevant dimensionless efficiency parameters (e.g. for turbulent dissipation) and hence α turb are bound to be slightly different, although the difference in α turb between 2D and 3D cannot be excessive given that the critical luminosity is very similar in both cases Dolence et al 2013;Couch 2013;Handy et al 2014). Moreover, since the record of 3D supernova simulations in obtaining explosions is mixed so far, and some crucial ingredients that boost the turbulent motions behind the shock may still be missing (such as strong seed perturbations from convective burning in the progenitor; Couch & Ott 2013;Couch et al 2015;, Finally, since our fits for the shock radius, and the advection and heating time-scales are already based on 2D and 3D simulations, and since the fits never perfectly reproduce the heating conditions in self-consistent models, α turb needs to be renormalised, and we will use values in the range α turb = 1.08 .…”

Section: Solution For the Shock Radiusmentioning

confidence: 99%

A simple approach to the supernova progenitor–explosion connection

Müller

Heger

Liptai

et al. 2016

Mon. Not. R. Astron. Soc.

207

376

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We present a new approach to understand the landscape of supernova explosion energies, ejected nickel masses, and neutron star birth masses. In contrast to other recent parametric approaches, our model predicts the properties of neutrino-driven explosions based on the precollapse stellar structure without the need for hydrodynamic simulations. The model is based on physically motivated scaling laws and simple differential equations describing the shock propagation, the contraction of the neutron star, the neutrino emission, the heating conditions, and the explosion energetics. Using model parameters compatible with multi-D simulations and a fine grid of thousands of supernova progenitors, we obtain a variegated landscape of neutron star and black hole formation similar to other parameterised approaches and find good agreement with semi-empirical measures for the "explodability" of massive stars. Our predicted explosion properties largely conform to observed correlations between the nickel mass and explosion energy. Accounting for the coexistence of outflows and downflows during the explosion phase, we naturally obtain a positive correlation between explosion energy and ejecta mass. These correlations are relatively robust against parameter variations, but our results suggest that there is considerable leeway in parametric models to widen or narrow the mass ranges for black hole and neutron star formation and to scale explosion energies up or down. Our model is currently limited to an all-or-nothing treatment of fallback and there remain some minor discrepancies between model predictions and observational constraints.

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TOWARD CONNECTING CORE-COLLAPSE SUPERNOVA THEORY WITH OBSERVATIONS. I. SHOCK REVIVAL IN A 15M_☉BLUE SUPERGIANT PROGENITOR WITH SN 1987A ENERGETICS

Cited by 46 publications

References 53 publications

Hydrodynamic simulations unravel the progenitor-supernova-remnant connection in SN 1987A

Hydrodynamic simulations unravel the progenitor-supernova-remnant connection in SN 1987A

A Two-Parameter Criterion for Classifying the Explodability of Massive Stars by the Neutrino-Driven Mechanism

A simple approach to the supernova progenitor–explosion connection

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TOWARD CONNECTING CORE-COLLAPSE SUPERNOVA THEORY WITH OBSERVATIONS. I. SHOCK REVIVAL IN A 15M☉BLUE SUPERGIANT PROGENITOR WITH SN 1987A ENERGETICS

Cited by 46 publications

References 53 publications

Hydrodynamic simulations unravel the progenitor-supernova-remnant connection in SN 1987A

Hydrodynamic simulations unravel the progenitor-supernova-remnant connection in SN 1987A

A Two-Parameter Criterion for Classifying the Explodability of Massive Stars by the Neutrino-Driven Mechanism

A simple approach to the supernova progenitor–explosion connection

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Product

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TOWARD CONNECTING CORE-COLLAPSE SUPERNOVA THEORY WITH OBSERVATIONS. I. SHOCK REVIVAL IN A 15M_☉BLUE SUPERGIANT PROGENITOR WITH SN 1987A ENERGETICS