Parametric studies of cosmic ray acceleration in supernova remnants

Kosenko, D.; Ferrand, Gilles; Decourchelle, A.

doi:10.1093/mnras/stu1251

Cited by 14 publications

(12 citation statements)

References 64 publications

(115 reference statements)

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“…The CR injection momentum parameter ξ can typically be in the range 3.0−4.5, where high values of ξ ≥ 4.0 correspond almost to the test-particle regime and low values of ξ ≤ 3.5 imply efficient DSA (Kosenko et al 2014). We adopt the common value ξ = 3.4, but also run simulations with ξ = 3.3 and ξ = 3.2 in order to study the sensitivity of the calculations to the value of this parameter.…”

Section: Resultsmentioning

confidence: 99%

Radio Evolution of Supernova Remnants Including Nonlinear Particle Acceleration: Insights from Hydrodynamic Simulations

Pavlović

Urošević

Арбутина

et al. 2018

ApJ

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We present a model for the radio evolution of supernova remnants (SNRs) obtained by using three-dimensional (3D) hydrodynamic simulations, coupled with nonlinear kinetic theory of cosmic ray (CR) acceleration in SNRs. We model the radio evolution of SNRs on a global level, by performing simulations for wide range of the relevant physical parameters, such as the ambient density, the supernova (SN) explosion energy, the acceleration efficiency and the magnetic field amplification (MFA) efficiency. We attribute the observed spread of radio surface brightnesses for corresponding SNR diameters to the spread of these parameters. In addition to our simulations of type Ia SNRs, we also considered SNR radio evolution in denser, nonuniform circumstellar environment, modified by the progenitor star wind. These simulations start with the mass of the ejecta substantially higher than in the case of a type Ia SN and presumably lower shock speed. The magnetic field is understandably seen as very important for the radio evolution of SNRs. In terms of MFA, we include both resonant and non-resonant modes in our large scale simulations, by implementing models obtained from first-principles, particle-in-cell (PIC) simulations and non-linear magnetohydrodynamical (MHD) simulations. We test the quality and reliability of our models on a sample consisting of Galactic and extragalactic SNRs. Our simulations give Σ−D slopes between -4 and -6 for the full Sedov regime. Recent empirical slopes obtained for the Galactic samples are around -5, while for the extragalactic samples are around -4.

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Section: Resultsmentioning

confidence: 99%

Radio Evolution of Supernova Remnants Including Nonlinear Particle Acceleration: Insights from Hydrodynamic Simulations

Pavlović

Urošević

Арбутина

et al. 2018

ApJ

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“…Note, that the oxygen abundance derived from the spectral fitting is about four times higher than in SNR 0509-67.5. The parametric studies (Kosenko, Ferrand & Decourchelle 2014) give n 0 = (0.5 − 1.0) cm −3 (for an explosion energy of 10 51 erg) and the light echo measurements of Rest et al (2005) indicate an age of 600 ± 200 yr.…”

Section: Oxygen In Supernova Remnants In the Large Magellanic Cloudmentioning

confidence: 98%

“…In order to confront the data with the models it is essential to know the dynamical properties and evolutionary stages of the remnants with sufficient accuracy. The analysis of SNR 0509-67.5 data reported by Kosenko et al (2008) gives an ISM density of n 0 = (0.4 − 0.6) cm −3 , Warren & Hughes (2004) measured n 0 = 1 Version 12.7.1 0.05 cm −3 , and an SNR parametric analysis reported in Kosenko, Ferrand & Decourchelle (2014) constrains n 0 to (0.1 − 0.3) cm −3 (for an SN explosion of 10 51 erg). Using light echo measurements Rest et al (2005) limited the age of SNR 0509-67.5 to 400 ± 120 yr. Measurements of Ghavamian et al (2007) give an age in the range 300 − 600 yr. Badenes et al (2008) suggested that the remnant originated 400 years ago and expands through an ISM with 0.4 cm −3 .…”

Section: Oxygen In Supernova Remnants In the Large Magellanic Cloudmentioning

confidence: 98%

Oxygen emission in remnants of thermonuclear supernovae as a probe for their progenitor system

Kosenko¹,

Hillebrandt²,

Kromer³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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Recent progress in numerical simulations of thermonuclear supernova explosions brings up a unique opportunity in studying the progenitors of Type Ia supernovae. Coupling state-ofthe-art explosion models with detailed hydrodynamical simulations of the supernova remnant evolution and the most up-to-date atomic data for X-ray emission calculations makes it possible to create realistic synthetic X-ray spectra for the supernova remnant phase. Comparing such spectra with high quality observations of supernova remnants could allow to constrain the explosion mechanism and the progenitor of the supernova. The present study focuses in particular on the oxygen emission line properties in young supernova remnants, since different explosion scenarios predict a different amount and distribution of this element. Analysis of the soft X-ray spectra from supernova remnants in the Large Magellanic Cloud and confrontation with remnant models for different explosion scenarios suggests that SNR 0509-67.5 could originate from a delayed detonation explosion and SNR 0519-69.0 from an oxygen-rich merger.

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“…For the remnants 0509-67.5 and 0519-69.0, the same method constrains the neutral hydrogen fraction in the surrounding ISM to >40%. The best-fitting ambient densities can be found from comparing the present size and ionization state of the remnant with hydrodynamical models: recently, Kosenko et al (2014) found n 0 = 0.1-0.3cm −3 for 0509-67.5, and n 0 = 1.0-2.0cm −3 for 0519-69.0, although Kosenko et al (2010) report densities as high as 2.4cm −3 . As a conservative estimate, we adopt 0.3cm −3 and 2.4cm −3 as our fiducial ISM densities for 0509-67.5 and 0519-69.0 respectively.…”

Section: Magellanic Supernova Remnantsmentioning

confidence: 99%

Balmer-dominated Shocks Exclude Hot Progenitors for Many Type Ia Supernovae

Woods

Ghavamian

Badenes

et al. 2018

ApJ

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The evolutionary mechanism underlying Type Ia supernova explosions remains unknown. Recent efforts to constrain progenitor models based on the influence that their high energy emission would have on the interstellar medium (ISM) of galaxies have proven successful. For individual remnants, Balmer-dominated shocks reveal the ionization state of hydrogen in the immediately surrounding gas. Here we report deep upper limits on the temperature and luminosity of the progenitors of four Type Ia remnants with associated Balmer filaments: SN 1006, 0509-67.5, 0519-69.0, and DEM L71. For SN 1006, existing observations of helium line emission in the diffuse emission ahead of the shock provide an additional constraint on the helium ionization state in the vicinity of the remnant. Using the photoionization code Cloudy, we show that these constraints exclude any hot, luminous progenitor for SN 1006, including stably hydrogen or helium nuclear-burning white dwarfs, as well as any Chandrasekhar-mass white dwarf accreting matter at 9.5 × 10 −8 M ⊙ /yr via a disk. For 0509-67.5, the Balmer emission alone rules out any such white dwarf accreting 1.4 × 10 −8 M ⊙ /yr. For 0519-69.0 and DEM L71, the inferred ambient ionization state of hydrogen is only weakly in tension with a recently hot, luminous progenitor, and cannot be distinguished from e.g., a relatively higher local Lyman continuum background, without additional line measurements. Future deep spectroscopic observations will resolve this ambiguity, and can either detect the influence of any luminous progenitor or rule out the same for all resolved SN Ia remnants.

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Parametric studies of cosmic ray acceleration in supernova remnants

Cited by 14 publications

References 64 publications

Radio Evolution of Supernova Remnants Including Nonlinear Particle Acceleration: Insights from Hydrodynamic Simulations

Radio Evolution of Supernova Remnants Including Nonlinear Particle Acceleration: Insights from Hydrodynamic Simulations

Oxygen emission in remnants of thermonuclear supernovae as a probe for their progenitor system

Balmer-dominated Shocks Exclude Hot Progenitors for Many Type Ia Supernovae

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