2014/07/31 by Danny Tsebrenko, Noam Soker · 25 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Astrophysics and Star Formation Studies #Ejecta #Gamma-ray bursts and supernovae #Nebula #Optics #Physics #Planetary nebula #Shock (circulatory) #Stars #Supernova #Supernova remnant #Synchrotron #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1093/mnras/stv669
published in Monthly Notices of the Royal Astronomical Society 450(2), 1399-1408 (Oxford University Press) · Revised version. 19 pages, 8 figures. Accepted to MNRAS
arxiv created 2015/04/16 · openalex publication_date 2015/04/24 · arxiv updated 2015/04/28 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Using 3D numerical hydrodynamical simulations we show that a Type Ia supernova (SN Ia) explosion inside a planetary nebula (PN) can explain the observed shape of the G1.9+0.3 supernova remnant (SNR) and its X-ray morphology. The SNR G1.9+0.3 morphology can be generally described as a sphere with two small and incomplete lobes protruding on opposite sides of the SNR, termed ‘ears’, a structure resembling many elliptical PNe. Observations show the synchrotron X-ray emission to be much stronger inside the two ears than in the rest of the SNR. We numerically show that a spherical SN Ia explosion into a circumstellar matter (CSM) with the structure of an elliptical PN with ears and clumps embedded in the ears can explain the X-ray properties of SNR G1.9+0.3. While the ejecta has already collided with the PN shell in most of the SNR and its forward shock has been slowed down, the ejecta is still advancing inside the ears. The fast forward shock inside the ears explains the stronger X-ray emission there. SN Ia inside PNe (SNIPs) seem to comprise a non-negligible fraction of resolved SN Ia remnants.