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Hydrodynamical and radio evolution of young supernova remnant G1.9+0.3 based on the model of diffusive shock acceleration

Pavlović, M. Z. (2017) Hydrodynamical and radio evolution of young supernova remnant G1.9+0.3 based on the model of diffusive shock acceleration. Monthly Notices of the Royal Astronomical Society, 468 (2). pp. 1616-1630. ISSN 0035-8711. https://resolver.caltech.edu/CaltechAUTHORS:20170227-101954539

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Abstract

The radio evolution of, so far the youngest known, Galactic supernova remnant (SNR) G1.9+0.3 is investigated by using three-dimensional (3D) hydrodynamic modelling and non-linear kinetic theory of cosmic ray (CR) acceleration in SNRs. We include consistent numerical treatment of magnetic field amplification (MFA) due to resonant streaming instability. Under the assumption that SNR G1.9+0.3 is the result of a Type Ia supernova explosion located near the Galactic Centre, using widely accepted values for explosion energy 10^(51) erg and ejecta mass 1.4 M⊙, the non-thermal continuum radio emission is calculated. The main purpose of this paper is to explain radio flux brightening measured over recent decades and also predict its future temporal evolution. We estimate that the SNR is now ∼120 yr old, expanding in an ambient density of 0.02 cm^(−3), and explain its steep radio spectral index only by means of efficient non-linear diffusive shock acceleration (NLDSA). We also make comparison between simulations and observations of this young SNR, in order to test the models and assumptions suggested. Our model prediction of a radio flux density increase of ∼1.8 per cent yr^(−1) during the past two decades agrees well with the measured values. We synthesize the synchrotron spectrum from radio to X-ray and it fits well the Very Large Array, Molonglo Observatory Synthesis Telescope, Effelsberg, Chandra and NuSTAR measurements. We also propose a simplified evolutionary model of the SNR in gamma rays and suggest it may be a promising target for gamma-ray observations at TeV energies with the future generation of instruments like Cherenkov Telescope Array. SNR G1.9+0.3 is the only known Galactic SNR with the increasing flux density and we present here the prediction that the flux density will start to decrease approximately 500 yr from now. We conclude that this is a general property of SNRs in the free expansion phase.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stx497DOIArticle
https://academic.oup.com/mnras/article/468/2/1616/3055708PublisherArticle
http://arxiv.org/abs/1702.07418arXivDiscussion Paper
Additional Information:© 2017 The Author. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 February 23. Received 2017 February 9; in original form 2016 December 28, Published: 27 February 2017. This work is part of project no. 176005 ‘Emission nebulae: structure and evolution’ supported by the Ministry of Education, Science, and Technological Development of the Republic of Serbia. Numerical simulations were run on the PARADOX-IV supercomputing facility at the Scientific Computing Laboratory of the Institute of Physics Belgrade, supported in part by the Ministry of Education, Science and Technological Development of the Republic of Serbia under projects no. ON171017 and OI1611005. Simulations were also run on cluster Jason, belonging to Automated Reasoning Group (ARGO) based at the Department of Computer Science, Faculty of Mathematics, University of Belgrade. I thank the anonymous referee for the very constructive suggestions on this manuscript. I would like to thank D. Urošević and B. Arbutina for introducing me into this exciting field, continually supporting and encouraging me, but also for the careful reviewing and editing of the typescript. I acknowledge the hospitality of the Osservatorio Astronomico di Palermo where part of this work was carried out, special thanks to Salvatore Orlando and Marco Miceli for their illuminating contributions to this project and also for reading the manuscript. I am grateful to Gilles Ferrand for the extremely helpful discussions, advices and help during this work and its coding. Brian Reville provided valuable discussions on different approaches in SNR modelling. I am indebted to Tara Murphy for kindly providing the currently available MOST radio flux densities, to Dr. Wolfgang Reich for providing Effelsberg radio data and to Rui-Zhi Yang and Leonid Ksenofontov for sharing the X-ray data for G1.9+0.3 and useful explanations. PLUTO is developed at the Turin Astronomical Observatory in collaboration with the Department of Physics of Turin University.
Group:NuSTAR
Subject Keywords:acceleration of particles – hydrodynamics – radiation mechanisms: non-thermal – cosmic rays – ISM: individual objects: G1.9+0.3 – ISM: supernova remnants
Issue or Number:2
Record Number:CaltechAUTHORS:20170227-101954539
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170227-101954539
Official Citation:M. Z. Pavlović; Hydrodynamical and radio evolution of young supernova remnant G1.9+0.3 based on the model of diffusive shock acceleration, Monthly Notices of the Royal Astronomical Society, Volume 468, Issue 2, 21 June 2017, Pages 1616–1630, https://doi.org/10.1093/mnras/stx497
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:74547
Collection:CaltechAUTHORS
Deposited By: Joy Painter
Deposited On:27 Feb 2017 18:43
Last Modified:03 Oct 2019 16:40

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