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

• Autores: Alsaberi, Rami Z. E.; Barnes, L. A.; Filipovic, Miroslav; Maxted, Nigel; Sano, H.; Rowell, Gavin; Bozzetto, L. M.; Gurovich, Sebastian; Urošević, D.; Onić, D.; For, B. Q.; Manojlović, P.; Wong, G.; Galvin, T. J.; Kavanagh, P.; Ralph, N. O.; Crawford, Evan; Sasaki, Manami; Haberl, Frank; Maggi, P.; Tothill, N. F. H.; Fukui, Y.
• Año de publicación: 2019
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: ISM: INDIVIDUAL OBJECTS: N 103B; ISM: SUPERNOVA REMNANTS; RADIO CONTINUUM: ISM; SUPERNOVAE: GENERAL
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

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