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

Autor: T. J. Galvin, Nicholas O Ralph, Nicholas F. H Tothill, Sebastián Gurovich, R. Z. E. Alsaberi, Hidetoshi Sano, P. Maggi, Miroslav Filipovic, Frank Haberl, Graeme F Wong, Manami Sasaki, Luke A. Barnes, Yasuo Fukui, P. Manojlovic, Gavin Rowell, Luke M Bozzetto, Dejan Urošević, Evan J Crawford, N. Maxted, D. Onić, Patrick J. Kavanagh, B. Q. For
Přispěvatelé: Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Rok vydání: 2019
Předmět:
Zdroj: Astrophysics and Space Science
Astrophysics and Space Science, Springer Verlag, 2019, 364 (11), ⟨10.1007/s10509-019-3696-8⟩
CONICET Digital (CONICET)
Consejo Nacional de Investigaciones Científicas y Técnicas
instacron:CONICET
ISSN: 0004-640X
1572-946X
DOI: 10.48550/arxiv.1911.04051
Popis: 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 200radm−2. However, we estimate the equipartition field to be of the order of ∼235 μG with an estimated minimum energy of Emin=6.3×1048erg. 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. Fil: Alsaberi, Rami Z. E.. University of Western Sydney; Australia Fil: Barnes, L. A.. University of Western Sydney; Australia Fil: Filipovic, Miroslav. University of Western Sydney; Australia Fil: Maxted, Nigel. University of Western Sydney; Australia. University of New South Wales; Australia Fil: Sano, H.. Nagoya University; Japón Fil: Rowell, Gavin. University of Adelaide; Australia Fil: Bozzetto, L. M.. University of Western Sydney; Australia Fil: Gurovich, Sebastian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba. Instituto de Astronomía Teórica y Experimental. Universidad Nacional de Córdoba. Observatorio Astronómico de Córdoba. Instituto de Astronomía Teórica y Experimental; Argentina Fil: Urošević, D.. Univerzitet U Beogradu; Serbia Fil: Onić, D.. Univerzitet U Beogradu; Serbia Fil: For, B. Q.. University of Western Australia; Australia. ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions; Australia Fil: Manojlović, P.. University of Western Sydney; Australia. CSIRO Astronomy and Space Sciences; Australia Fil: Wong, G.. University of Western Sydney; Australia. CSIRO Astronomy and Space Sciences; Australia Fil: Galvin, T. J.. Curtin University. International Centre for Radio Astronomy Research; Australia. University of Western Sydney; Australia. CSIRO Astronomy and Space Sciences; Australia Fil: Kavanagh, P.. Dublin Institute for Advanced Studies; Irlanda Fil: Ralph, N. O.. University of Western Sydney; Australia Fil: Crawford, Evan. University of Western Sydney; Australia Fil: Sasaki, Manami. Universitat Erlangen-Nuremberg; Alemania Fil: Haberl, Frank. Institut Max Planck Fuer Gesellschaft. Max Planck Institute For Extraterrestrial Physics; Alemania Fil: Maggi, P.. Université de Strasbourg; Francia. Centre National de la Recherche Scientifique; Francia Fil: Tothill, N. F. H.. University of Western Sydney; Australia Fil: Fukui, Y.. University of Adelaide; Australia
Databáze: OpenAIRE
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