Progenitor Model of SN 1987A Based on the Slow Merger Scenario

Abstract

Even after elaborate investigations for 30 years, we still do not know well how the progenitor of SN 1987A has evolved. To explain unusual red-to-blue evolution, previous studies suggest that in a red giant stage either the increase of surface He abundance or the envelope mass was necessary. It is usually supposed that the He enhancement is caused by the rotational mixing, and the mass increase is by a binary merger. Thus, we have investigated these scenarios thoroughly. The obtained findings are that rotating single star models do not satisfy all the observational constraints and that the enhancement of envelope mass alone does not explain observations. Here, we consider a slow merger scenario in which both the He abundance and the envelope mass enhancements are expected to occur. We indeed show that most observational constraints such as the red-to-blue evolution, lifetime, total mass, position in the HR diagram at collapse, and the chemical anomalies are well reproduced by the merger model of 14 and 9 M${}_{\odot }$ stars. We also discuss the effects of the added envelope spin in the merger scenarios.

2 figures and 1 table. Accepted for publication in MNRAS LETTER

References in corpus (4)

• The Triple-Ring Nebula around SN1987A: Fingerprint of a binary merger
• Stellar Yields of Rotating First Stars. I. Yields of Weak Supernovae and Abundances of Carbon-enhanced Hyper Metal Poor Stars
• The quest for blue supergiants: binary merger models for the evolution of the progenitor of SN 1987A
• On the Progenitor of Supernova 1987A

Cited by in corpus (22)

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• Modeling of Magneto-Rotational Stellar Evolution I. Method and first applications
• Matter Mixing in Aspherical Core-collapse Supernovae: Three-dimensional Simulations with Single Star and Binary Merger Progenitor Models for SN 1987A
• Three-dimensional simulation of a core-collapse supernova for a binary star progenitor of SN 1987A
• Pre-supernova evolution and final fate of stellar mergers and accretors of binary mass transfer
• Supernova 1987A: 3D Mixing and light curves for explosion models based on binary-merger progenitors
• Indication of a Pulsar Wind Nebula in the hard X-ray emission from SN 1987A
• The Re-Acceleration of the Shock Wave in the Radio Remnant of SN 1987A
• Additional evidence for a pulsar wind nebula in the heart of SN 1987A from multi-epoch X-ray data and MHD modeling
• The influence of line opacity treatment in STELLA on supernova light curves
• X-ray Absorption in Young Core-Collapse Supernova Remnants
• Constraining the overcontact phase in massive binary evolution -- II. Period stability of known O+O overcontact systems
• Intermediate Luminosity Optical Transients (ILOTs) from merging giants
• The morphology of the ejecta of SN 1987A at 31 years from 1150 to 10000 Å
• Tracing the ejecta structure of SN 1987A: Insights and diagnostics from 3D MHD simulations
• Investigating Time Evolution of Thermal Emission from the Putative Neutron Star in SN 1987A for 50+ Years
• Polarized radio emission unveils the structure of the pre-supernova circumstellar magnetic field and the radio emission in SN1987A
• Near-infrared evolution of the equatorial ring of SN 1987A
• Possible post-kick jets in SN 1987A
• Detailed evolutionary models of massive contact binaries: I. Model grids and synthetic populations for the Magellanic Clouds
• Measuring the initial mass of 44Ti in SN 1987A through the 44Sc emission line