Discovery of Double-Ring Structure in the Supernova Remnant N103B: Evidence for Bipolar Winds from a Type Ia Supernova Progenitor

TL;DR

This study reveals a double-ring structure in the supernova remnant N103B, indicating bipolar ejecta expansion likely caused by a dense circumstellar torus from a single-degenerate Type Ia supernova progenitor.

Contribution

The paper introduces a novel feature extraction method applied to X-ray data, uncovering a double-ring structure and bipolar bubbles in N103B, providing new insights into progenitor evolution.

Findings

Double-ring structure in IME ejecta

Bimodal ionization state distribution

Evidence for a dense CSM torus

Abstract

The geometric structure of supernova remnants (SNR) provides a clue to unveiling the pre-explosion evolution of their progenitors. Here we present an X-ray study of N103B (0509-68.7), a Type Ia SNR in the Large Magellanic Cloud, that is known to be interacting with dense circumstellar matter (CSM). Applying our novel method for feature extraction to deep Chandra observations, we have successfully resolved the CSM, Fe-rich ejecta, and intermediate-mass element (IME) ejecta components, and revealed each of their spatial distribution. Remarkably, the IME ejecta component exhibits a double-ring structure, implying that the SNR expands into an hourglass-shape cavity and thus forms bipolar bubbles of the ejecta. This interpretation is supported by more quantitative spectroscopy that reveals a clear bimodality in the distribution of the ionization state of the IME ejecta. These observational results can be naturally explained if the progenitor binary system had formed a dense CSM torus on the orbital plane prior to the explosion, providing further evidence that the SNR N103B originates from a single-degenerate progenitor.