Radio emission from interstellar shocks: Young type Ia supernovaremnants and 
the case of N 103B in the Large Magellanic Cloud

Alsaberi, R. Z. E.; Barnes, L. A.; Filipović, M. D.; Maxted, N. I.; Sano, H.; Rowell, G.; Bozzetto, L. M.; Gurovich, S.; Urošević, D.; Onić, D.; For, B.-Q.; Manojlović, P.; Wong, G.; Galvin, T. J.; Kavanagh, P.; Ralph, N. O.; Crawford, E. J.; Sasaki, M.; Haberl, F.; Maggi, P.; Tothill, N. F. H.; Fukui, Y.

doi:10.1007/s10509-019-3696-8

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Radio emission from interstellar shocks: Young type Ia supernovaremnants and the case of N 103B in the Large Magellanic Cloud

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Haberl, F.
High Energy Astrophysics, MPI for Extraterrestrial Physics, Max Planck Society;

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Citation

Alsaberi, R. Z. E., Barnes, L. A., Filipović, M. D., Maxted, N. I., Sano, H., Rowell, G., et al. (2019). Radio emission from interstellar shocks: Young type Ia supernovaremnants and the case of N 103B in the Large Magellanic Cloud. Astrophysics and Space Science, 364(11): 204. doi:10.1007/s10509-019-3696-8.

Cite as: https://hdl.handle.net/21.11116/0000-0006-4223-8

Abstract

We investigate young type Ia supernova remnants (SNRs) in our Galaxy and neighbouring galaxies in order to understand their properties and early stage of their evolution. Here we present a radio continuum study based on new and archival data from the Australia Telescope Compact Array (ATCA) 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 (SD) 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 (NLDSA) effects or presence of two different populations of ultra-relativistic electrons.
We also note unpolarised 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 μG for an average rotation measurement of 200 rad m⁻²
. However, we estimate the equipartition field to be of the order of ∼235 μG with an estimated minimum energy of E_min=6.3×10⁴⁸ erg. The close (∼0.5^∘
) 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.