Expansion measurement of Supernova Remnant RX J1713.7-3946

Abstract

Supernova remnant (SNR) RX J1713.7-3946 is well known for its bright TeV gamma-ray emission with shell-like morphology. To constrain the hydrodynamical evolution, we have performed six times observations of the northwestern (NW) shell with the Chandra X-ray Observatory from 2005 to 2011, and measured the proper motion by using these data and the first epoch observation taken in 2000. The blast-wave shock speed at the NW shell is measured to be $(3900\pm 300)(d/\mathrm{kpc})\mathrm{km}{\mathrm{s}}^{-1}$ with an estimated distance of $d=1$ kpc, and the proper motions of other structures within the NW shell are significantly less than that. Assuming that the measured blast-wave shock speed is the representative of the remnant's outer shock wave as a whole, we have confronted our measurements as well as a recent detection of thermal X-ray lines, with the analytic solution of the hydrodynamical properties of SNRs. Our hydrodynamical analysis indicates that the age of the remnant is 1580-2100 years, supporting the association with SN393. A model with SN kinetic energy of $E=10^{51}\mathrm{erg}$, the ejecta mass of $M_{\mathrm{ej}}=3M_{\odot }$, and the ambient density at the current blast wave location of $n_2=0.015{\mathrm{cm}}^{-3}$, provides reasonable explanation for our measurements and previous findings at the X-ray and gamma-ray wavelengths. We find that the transition to the Sedov-Taylor (ST) phase is incomplete for any reasonable set of parameters, implying that the current maximum energy of accelerated protons in RX J1713.7-3946 would not correspond to the maximum attainable energy for this remnant.

arXiv comment11 pages, 9 figures, 5 tables; Accepted for publication in PASJ

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• X-ray bounds on cooling, composition, and magnetic field of the Cassiopeia A neutron star and young central compact objects
• TeV cosmic ray nuclei acceleration in shell-type supernova remnants with hard $\gamma$-ray spectra
• ALMA CO Observations of the Gamma-Ray Supernova Remnant RX J1713.7-3946: Discovery of Shocked Molecular Cloudlets and Filaments at 0.01 pc scales
• Shock-Cloud Interaction in the Southwestern Rim of RX J1713.7$-$3946 Evidenced by Chandra X-ray Observations
• The interstellar medium in young supernova remnants: key to the production of cosmic X-rays and $\gamma$-rays
• A kinematic study of central compact objects and their host supernova remnants
• NuSTAR observations of the supernova remnant RX J1713.7$-$3946
• Time evolution of broadband non-thermal emission from supernova remnants in different circumstellar environments
• A Laminar Model for the Magnetic Field Structure in Bow-Shock Pulsar Wind Nebulae
• Observational constraints on the maximum energies of accelerated particles in supernova remnants: low maximum energies and a large variety
• Discovery of a shock-compressed magnetic field in the north-western rim of the young supernova remnant RX J1713.7-3946 with X-ray polarimetry
• LMC N132D: A mature supernova remnant with a power-law gamma-ray spectrum extending beyond 8 TeV
• Simulating TeV gamma-ray morphologies of shell-type supernova remnants
• Spatially resolved spectroscopy of nonthermal X-rays in RX J1713.7-3946 with Chandra
• What causes the absence of pulsations in Central Compact Objects in Supernova Remnants?
• Long-term evolution of non-thermal emission from Type Ia and core-collapse supernova remnants in a diversified circumstellar medium
• X-ray Hotspots in the Northwest Shell of the Supernova Remnant RX J1713.7$-$3946
• Possible Detection of X-Ray Emitting Circumstellar Material in the Synchrotron-Dominated Supernova Remnant RX J 1713.7-3946
• Searches for continuous gravitational waves from young supernova remnants in the early third observing run of Advanced LIGO and Virgo
• Expansion and ongoing cosmic ray acceleration in HESS J1731-347
• Radial Profiles of Non-thermal Emission from Supernova Remnant RX J1713.7-3946
• Survival of Molecular Complexity under Recent Supernova Feedback: Detection of Hot Cores in RX J1713.7-3946