The 30 Year Search for the Compact Object in SN 1987A

Alp, Dennis; Larsson, Josefin; Fransson, Claes; Indebetouw, R.; Jerkstrand, A.; Ahola, Antero; Burrows, D. N.; Challis, P.; Cigan, Phil; Cikota, Aleksandar; Kirshner, R.; Loon, J. Th. van; Mattila, S.; Ng, C.‐Y.; Park, Sangwook; Spyromilio, J.; Woosley, S. E.; Baes, M.; Bouchet, P.; Chevalier, Roger A.; Frank, Kari A.; Gaensler, B. M.; Gomez, Haley Louise; Janka, Hans-Thomas; Leibundgut, B.; Lundqvist, Peter; Marcaide, J. M.; Matsuura, M.; Sollerman, J.; Sonneborn, G.; Staveley‐Smith, L.; Zanardo, Giovanna; Gabler, Michael; Taddia, F.; Wheeler, J. C.

doi:10.3847/1538-4357/aad739

Cited by 49 publications

(49 citation statements)

References 184 publications

(253 reference statements)

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“…We ignored such a progenitor rotation because it is so slow that it does not affect the neutrino-driven mechanism, nor is it an efficient energy source for a magnetohydrodynamics mechanism. This is consistent with the lack of any bright pulsar in the current remnant (Alp et al 2018), which supports slow rotation of the degenerate stellar core. Therefore a scenario involving the formation of (jittering) jets (Soker 2017;Bear & Soker 2018) seems disfavored as well.…”

Section: Discussionsupporting

confidence: 87%

Three-dimensional mixing and light curves: constraints on the progenitor of supernova 1987A

Utrobin

Wongwathanarat

Janka

et al. 2019

A&A

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With the same method as used previously, we investigate neutrino-driven explosions of a larger sample of blue supergiant models. The blue supergiants were evolved as single-star progenitors. The larger sample includes three new presupernova stars. The results are compared with light-curve observations of the peculiar type IIP supernova 1987A (SN 1987A). The explosions were modeled in 3D with the neutrino-hydrodynamics code Prometheus-HOTB, and light-curve calculations were performed in spherical symmetry with the radiation-hydrodynamics code Crab, starting at a stage of nearly homologous expansion. Our results confirm the basic findings of the previous work: 3D neutrino-driven explosions with SN 1987A-like energies synthesize an amount of 56 Ni that is consistent with the radioactive tail of the light curve. Moreover, the models mix hydrogen inward to minimum velocities below 400 km s −1 as required by spectral observations and a 3D analysis of molecular hydrogen in SN 1987A. Hydrodynamic simulations with the new progenitor models, which possess smaller radii than the older ones, show much better agreement between calculated and observed light curves in the initial luminosity peak and during the first 20 days. A set of explosions with similar energies demonstrated that a high growth factor of Rayleigh-Taylor instabilities at the (C+O)/He composition interface combined with a weak interaction of fast Rayleigh-Taylor plumes, where the reverse shock occurs below the He/H interface, provides a sufficient condition for efficient outward mixing of 56 Ni into the hydrogen envelope. This condition is realized to the required extent only in one of the older stellar models, which yielded a maximum velocity of around 3000 km s −1 for the bulk of ejected 56 Ni, but failed to reproduce the helium-core mass of 6 M inferred from the absolute luminosity of the presupernova star. We conclude that none of the single-star progenitor models proposed for SN 1987A to date satisfies all constraints set by observations.

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Section: Discussionsupporting

confidence: 87%

Three-dimensional mixing and light curves: constraints on the progenitor of supernova 1987A

Utrobin

Wongwathanarat

Janka

et al. 2019

A&A

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“…Currently the newly formed neutron star (if any) has not been detected yet. This is probably due to heavy absorption of its emission caused by a high local absorbing column density along the LoS (Orlando et al 2015;Alp et al 2018). Future detection of the neutron star in SN 1987A will provide a strong constraint on the initial large-scale asymmetry and on the mechanism of neutron star kick.…”

Section: Discussionmentioning

confidence: 99%

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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“…The compact object of SN 1987A has not been detected yet but it could be a thermally emitting NS obscured by dust (Orlando et al 2015;Alp et al 2018). If the explosion of SN 1987A was an asymmetric one as demonstrated in the models, e.g., b18.3-high, the compact object (probably NS) could have been kicked to the opposite direction to the motion of the bulk of the supernova ejecta.…”

Section: Neutron Star Kick Velocitymentioning

confidence: 99%

Matter Mixing in Aspherical Core-collapse Supernovae: Three-dimensional Simulations with Single-star and Binary Merger Progenitor Models for SN 1987A

Ono

Nagataki

Ferrand

et al. 2020

ApJ

104

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We perform three-dimensional hydrodynamic simulations of aspherical core-collapse supernovae focusing on the matter mixing in SN 1987A. The impacts of four progenitor (pre-supernova) models and parameterized aspherical explosions are investigated. The four pre-supernova models include a blue supergiant (BSG) model based on a slow merger scenario developed recently for the progenitor of SN 1987A (Urushibata et al. 2018. The others are a BSG model based on a single star evolution and two red supergiant (RSG) models. Among the investigated explosion (simulation) models, a model with the binary merger progenitor model and with an asymmetric bipolar-like explosion, which invokes a jetlike explosion, best reproduces constraints on the mass of high velocity 56 Ni, as inferred from the observed [Fe II] line profiles. The advantage of the binary merger progenitor model for the matter mixing is the flat and less extended ρ r 3 profile of the C+O core and the helium layer, which may be characterized by the small helium core mass. From the best explosion model, the direction of the bipolar explosion axis (the strongest explosion direction), the neutron star (NS) kick velocity, and its direction are predicted. Other related implications and future prospects are also given.

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The 30 Year Search for the Compact Object in SN 1987A

Cited by 49 publications

References 184 publications

Three-dimensional mixing and light curves: constraints on the progenitor of supernova 1987A

Three-dimensional mixing and light curves: constraints on the progenitor of supernova 1987A

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

Matter Mixing in Aspherical Core-collapse Supernovae: Three-dimensional Simulations with Single-star and Binary Merger Progenitor Models for SN 1987A

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