Non-thermal radiation from Type Ia supernova remnants

Edmon, Paul; Kang, Hyesung; Jones, T. W.; Ma, Renyi

doi:10.1111/j.1365-2966.2011.18652.x

Cited by 22 publications

(25 citation statements)

References 61 publications

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“…For example, p e,br (t) decreases from 10 2.8 m p c to 10 2.5 m p c for t/t o = 0.5 − 5 in W1 model. The peak of G e (p) near p e,max comes from the electron population in the upstream region, which cools much less efficiently due to weaker magnetic field there (Edmon et al 2011). Because of the same reason, the X-ray synchrotron emission due to this population of upstream electrons would be much less pronounced, compared to the electron energy spectrum.…”

Section: Dsa Simulation Resultsmentioning

confidence: 98%

“…We set B r = 6.5 µG, including the cosmic background and mean Galactic radiation fields (Edmon et al 2011). The cooling term is set to be b(p) = 0 for protons.…”

Section: Crash Code For Dsamentioning

confidence: 99%

“…Multi-band observations of nonthermal emissions from radio to γ-ray have provided a powerful tool to examine theoretical models of nonlinear DSA at SNRs (e.g., Berezhko & Völk 1997;Berezhko et al 2009Berezhko et al , 2012Caprioli 2011;Edmon et al 2011). For example, radio spectral index carries the information on the power-law portion of ∼ GeV electrons, while X-ray continuum reflects the exponential cut-off near the maximum electron energy, E e,max ∼ 10 TeV, and the magnetic field strength.…”

Section: Introductionmentioning

confidence: 99%

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Effects of Wave-Particle Interactions on Diffusive Shock Acceleration at Supernova Remnants

Kang¹

2013

Journal of The Korean Astronomical Society

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Nonthermal radiation from supernova remnants (SNRs) provides observational evidence and constraints on the diffusive shock acceleration (DSA) hypothesis for the origins of Galactic cosmic rays (CRs). Recently it has been recognized that a variety of plasma wave-particle interactions operate at astrophysical shocks and the detailed outcomes of DSA are governed by their complex and nonlinear interrelationships. Here we calculate the energy spectra of CR protons and electrons accelerated at Type Ia SNRs, using time-dependent, DSA simulations with phenomenological models for magnetic field amplification due to CR streaming instabilities, Alfvénic drift, and free escape boundary. We show that, if scattering centers drift with the Alfvén speed in the amplified magnetic fields, the CR energy spectrum is steepened and the acceleration efficiency is significantly reduced at strong CR modified SNR shocks. Even with fast Afvénic drift, DSA can still be efficient enough to develop a substantial shock precursor due to CR pressure feedback and convert about 20-30% of the SN explosion energy into CRs. Since the high energy end of the CR proton spectrum is composed of the particles that are injected in the early stages, in order to predict nonthermal emissions, especially in X-ray and γ-ray bands, it is important to follow the time dependent evolution of the shock dynamics, CR injection process, magnetic field amplification, and particle escape. Thus it is crucial to understand the details of these plasma interactions associated with collisionless shocks in successful modeling of nonlinear DSA.

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Section: Dsa Simulation Resultsmentioning

confidence: 98%

“…We set B r = 6.5 µG, including the cosmic background and mean Galactic radiation fields (Edmon et al 2011). The cooling term is set to be b(p) = 0 for protons.…”

Section: Crash Code For Dsamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Effects of Wave-Particle Interactions on Diffusive Shock Acceleration at Supernova Remnants

Kang¹

2013

Journal of The Korean Astronomical Society

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“…Contrary to what is widely considered, SNR RX J1713.7−3946 is not in the ST stage. Because the total energy content of cosmic rays has to be large enough to produce the observed gamma rays regardless of the emission models (see Edmon et al 2011), a very young evolutional stage in Models 1, 2, 9, and 10 where tage ≪ tST would be inappropriate.…”

Section: Evolutional Phasementioning

confidence: 99%

Expansion measurements of supernova remnant RX J1713.7−3946

Tsuji¹,

Uchiyama²

2016

Publications of the Astronomical Society of Japan

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Supernova remnant (SNR) RX J1713.7−3946 is well known for its bright TeV gamma-ray emission with shell-like morphology. Strong synchrotron X-ray emission dominates the total X-ray flux in SNR RX J1713.7−3946 and the X-ray morphology is broadly similar to the TeV gammaray appearance. The synchrotron X-ray and TeV gamma-ray brightness allows us to perform detailed analysis of the acceleration of TeV-scale particles in this SNR. To constrain the hydrodynamical evolution of RX J1713.7−3946, 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 ± 300)(d/kpc) km swith 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 erg, the ejecta mass of M ej = 3 M ⊙ , and the ambient density at the current blast wave location of n 2 = 0.015 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.

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“…To compute the non-thermal emission of particles, we use the general-purpose code AURA (P. P. Edmon, 2012, private communication), which is a rewrite of the code COSMICP presented in Edmon et al (2011). It makes use of the formalism of Schlickeiser (2002) for leptonic processes, and of the formalism of Kelner et al (2006) and Kelner & Aharonian (2008) for hadronic processes.…”

Section: Particle Emissionmentioning

confidence: 99%

Three-Dimensional Simulations of the Non-Thermal Broadband Emission From Young Supernova Remnants Including Efficient Particle Acceleration

Ferrand

Decourchelle

Safi‐Harb

2014

ApJ

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Supernova remnants are believed to be major contributors to Galactic cosmic rays. In this paper, we explore how the non-thermal emission from young remnants can be used to probe the production of energetic particles at the shock (both protons and electrons). Our model couples hydrodynamic simulations of a supernova remnant with a kinetic treatment of particle acceleration. We include two important back-reaction loops upstream of the shock: energetic particles can (1) modify the flow structure and (2) amplify the magnetic field. As the latter process is not fully understood, we use different limit cases that encompass a wide range of possibilities. We follow the history of the shock dynamics and of the particle transport downstream of the shock, which allows us to compute the non-thermal emission from the remnant at any given age. We do this in three dimensions, in order to generate projected maps that can be compared with observations. We observe that completely different recipes for the magnetic field can lead to similar modifications of the shock structure, although to very different configurations of the field and particles. We show how this affects the emission patterns in different energy bands, from radio to X-rays and γ -rays. High magnetic fields (>100 μG) directly impact the synchrotron emission from electrons, by restricting their emission to thin rims, and indirectly impact the inverse Compton emission from electrons and also the pion decay emission from protons, mostly by shifting their cut-off energies to respectively lower and higher energies.

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Non-thermal radiation from Type Ia supernova remnants

Cited by 22 publications

References 61 publications

Effects of Wave-Particle Interactions on Diffusive Shock Acceleration at Supernova Remnants

Effects of Wave-Particle Interactions on Diffusive Shock Acceleration at Supernova Remnants

Expansion measurements of supernova remnant RX J1713.7−3946

Three-Dimensional Simulations of the Non-Thermal Broadband Emission From Young Supernova Remnants Including Efficient Particle Acceleration

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