First 3D Morpho-Kinematic model of Supernova Remnants. The case of VRO 42.05.01 (G 166.0+4.3)

Abstract

We present the first three dimensional (3D) Morpho-Kinematic (MK) model of a supernova remnant (SNR), using as a case study the Galactic SNR VRO 42.05.01. We employed the astrophysical code SHAPE in which wide field imaging and high resolution spectroscopic data were utilized, to reconstruct its 3D morphology and kinematics. We found that the remnant consists of three basic distinctive components that we call: a "shell", a "wing" and a "hat". With respect to their kinematical behaviour, we found that the "wing" and the "shell" have similar expansion velocities (V exp = $115$$\pm 5$ km/s). The "hat" presents the lowest expansion velocity of the remnant (V exp = $90$$\pm 20$ km/s), while the upper part of the "shell" presents the highest velocity with respect to the rest of the remnant (V exp = $155$$\pm 15$ km/s). Furthermore, the whole nebula has an inclination of ~$3°-5°$ with respect to the plane of the sky and a systemic velocity of V sys = -$17$$\pm 3$ km/s . We discuss the interpretation of our model results regarding the origin and evolution of the SNR and we suggest that VRO 42.05.01 had an interaction history with an inhomogeneous ambient medium most likely shaped by the mass outflows of its progenitor star.

6 pages, 3 figures, 1 animated video of the 3D model, accepted for publication in MNRAS

References in corpus (6)

• Very Deep Inside the SN 1987A Core Ejecta: Molecular Structures Seen in 3D
• Multi-dimensional simulations of the expanding supernova remnant of SN 1987A
• The Three-Dimensional Expansion of the Ejecta from Tycho's Supernova Remnant
• High velocity string of knots in the outburst of the Planetary Nebula Hb4
• The environment of supernova remnant VRO 42.05.01 as probed with IRAM 30m molecular line observations
• Distance mapping applied to four well-known planetary nebulae and a nova shell

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