2017/04/30 by Conor M. B. Omand, Kazumi Kashiyama, Kohta Murase · 1 citation
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Crab Nebula #Galaxy #Gamma-ray bursts and supernovae #Jansky #Light curve #Magnetar #Nebula #Neutron star #Physics #Pulsar #Pulsar wind nebula #Pulsars and Gravitational Waves Research #Radio galaxy #Stars #Supernova #Supernova remnant #astro-ph.HE
paper · pdf · doi:10.1093/mnras/stx2743
published as Mon.Not.Roy.Astron.Soc. 474 (2018) 573 · 8 pages, 6 figures, accepted by MNRAS
arxiv created 2017/10/18 · openalex publication_date 2017/10/19 · arxiv updated 2017/12/15 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
It has been widely argued that Type-I superluminous supernovae (SLSNe-I) are driven by powerful central engines with a long-lasting energy injection after the core-collapse of massive progenitors. One of the popular hypotheses is that the hidden engines are fast-rotating pulsars with a magnetic field of B ∼ 1013–1015 G. Murase, Kashiyama & Mészáros proposed that quasi-steady radio/submm emission from non-thermal electron–positron pairs in nascent pulsar wind nebulae can be used as a relevant counterpart of such pulsar-driven supernovae (SNe). In this work, focusing on the nascent SLSN-I remnants, we examine constraints that can be placed by radio emission. We show that the Atacama Large Millimeter/submillimetre Array can detect the radio nebula from SNe at DL ∼ 1 Gpc in a few years after the explosion, while the Jansky Very Large Array can also detect the counterpart in a few decades. The proposed radio follow-up observation could solve the parameter degeneracy in the pulsar-driven SN model for optical/UV light curves, and could also give us clues to young neutron star scenarios for SLSNe-I and fast radio bursts.