Radio Emission from Interstellar Shocks: Young Type Ia Supernova Remnants and the Case of N 103B in the Large Magellanic Cloud

TL;DR

This study presents a detailed radio analysis of the young Type Ia supernova remnant N 103B in the LMC, revealing asymmetrical morphology, spectral features, and magnetic field estimates, contributing to understanding supernova explosion mechanisms.

Contribution

It provides new radio continuum observations and analysis of N 103B, highlighting asymmetrical morphology, spectral properties, and magnetic fields, and compares these features with other young Type Ia SNRs to infer explosion scenarios.

Findings

Radio spectral index of -0.75 consistent with young Type Ia SNRs

Radial polarisation peak observed at 5500 and 9000 MHz

Magnetic field strength estimated at 16.4 microG

Abstract

Here we present a radio continuum study based on new and archival data from the Australia Telescope Compact Array towards N 103B, a young (<=1000 yrs) spectroscopically confirmed type Ia SNR in the Large Magellanic Cloud (LMC) and proposed to have originated from a single degenerate progenitor. The radio morphology of this SNR is asymmetrical with two bright regions towards the north-west and south-west of the central location as defined by radio emission. N 103B identified features include: a radio spectral index of -0.75+-0.01 (consistent with other young type Ia SNRs in the Galaxy); a bulk SNR expansion rate as in X-rays; morphology and polarised electrical field vector measurements where we note radial polarisation peak towards the north-west of the remnant at both 5500 and 9000 MHz. The spectrum is concave-up and the most likely reason is the non-linear diffusive shock acceleration effects or presence of two different populations of ultra-relativistic electrons. We also note unpolarized clumps near the south-west region which is in agreement with this above scenario. We derive a typical magnetic field strength for N 103B, of 16.4 microG for an average rotation measurement of 200 rad m^-2. However, we estimate the equipartition field to be of the order of ~235 microG with an estimated minimum energy of Emin=6.3*10^48 erg. The close (~0.5 degree) proximity of N 103B to the LMC mid-plane indicates that an early encounter with dense interstellar medium may have set an important constrain on SNR evolution. Finally, we compare features of N 103B, to six other young type Ia SNRs in the LMC and Galaxy, with a range of proposed degeneracy scenarios to highlight potential differences due to a different models. We suggest that the single degenerate scenario might point to morphologically asymmetric type Ia supernova explosions.