The interaction of the supernova remnant VRO 42.05.01 with its H I environment

Radio emission from supernova remnants

“…An example of this type is the SNR VRO 42.05.01 (G166.0+4.3) ( Fig. 3 Upper-right), that at first sight appears to be two different sources adjoining in the plane of the sky (Landecker et al 1982) but that HI observations demonstrated that it is a single SNR breaking out from a warm medium into a tenuous interstellar cavity (Pineault et al 1987;Landecker et al 1989); barrel-shaped or bilateral: SNRs characterized by a clear axis of symmetry, low level of emission along this axis, and two bright limbs on either sides (Gaensler 1998). Typical examples of this type are G296.5+10.0 (Giacani et al 2000) and SN1006 (Reynolds & Gilmore 1986;Petruk et al 2009) (Fig.…”

Radio spectral index study of the SNRs OA184 and VRO42.05.01

“…The most reliable estimate is 4.5 ± 1.5 kpc by Landecker et al (1989) based on HI measurements. The latter yields a radius for OA184 of 50 pc.…”

“…The shell has a radius of 25 pc, for a distance of 5 kpc, and the SNR is currently in its isothermal stage (Pineault et al 1987). The SNR is interacting with an HI cloud and is inside an expanding HI shell, which yields a more reliable distance of 4.5 ± 1.5 kpc (Landecker et al 1989). Burrows & Guo (1994) present the first X-ray images of VRO.42.05.01: in X-rays it is center-filled.…”

VRO 42.05.01: A supernova remnant resulted by a supersonic, mass losing progenitor star

“…These models consider that VRO occurred close to the contact discontinuity of two interstellar media with different properties. According to them, the portion of the remnant that is evolving in the denser medium forms the 'shell', while the 'wing' results by the SNR 's breakout into the more tenuous medium (Pineault et al, 1985;Landecker et al, 1989). Arias et al (2019b) added an extra ingredient to these models suggesting that the progenitor of VRO was a runaway star.…”