The theory of synchrotron emission from supernova remnants

Berezhko, E. G.; Völk, H. J.

doi:10.1051/0004-6361:20041111

Cited by 131 publications

(232 citation statements)

References 48 publications

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“…From the position of MCSNR J0536-7038 at the surface brightness to diameter (Σ -D) diagram ((D, Σ) = (32 pc, 3.6 × 10 −21 W m −2 Hz −1 sr −1 )) by Berezhko & Völk (2004), we can estimate that the remnant is likely to be an SNR in the late energy conserving phase, with an explosion energy between 0.25 and 1 × 10 51 ergs, which evolves in an environment of density ∼1 cm −3 .…”

Section: Resultsmentioning

confidence: 99%

Radio-continuum study of MCSNR J0536–7038 (DEM L249)

Bozzetto¹,

Filipović²

2014

Astrophys Space Sci

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We present a detailed radio-continuum study on Australia Telescope Compact Array (ATCA) observations of Large Magellanic Cloud (LMC) supernova remnant (SNR), MCSNR J0536-7038. This Type Ia SNR follows a horseshoe morphology, with a size 32 pc × 32 pc (1-pc uncertainty in each direction). It exhibits a radio spectrum α = −0.52 ± 0.07 between λ = 73 and 6 cm. We report detections of regions showing moderately high fractional polarisation at 6 cm, with a peak value of 71±25% and a mean fractional polarisation of 35±8%. We also estimate an average rotation measure across the remnant of -237 rad m −2 . The intrinsic magnetic field appears to be uniformly distributed, extending in the direction of the two brightened limbs of the remnant.

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Section: Resultsmentioning

confidence: 99%

Radio-continuum study of MCSNR J0536–7038 (DEM L249)

Bozzetto¹,

Filipović²

2014

Astrophys Space Sci

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“…At least, with the ambient density of nHI ≃ 0.3 cm −3 the ring nebula fits well the empirical evolutionary sequence of SNRs on the log(vexp) versus log(Rs(nHI) 1/3 ) plot suggested by Lozinskaya (1980a,b). The expected radio surface brightness of an SNR 210 pc in diameter is about Σ1GHz = 10 −22 − 10 −21 Wm −2 Hz −1 sr −1 (see the Σ−D relation in Lozinskaya 1981; Berezhko & Volk 2004;Asvarov 2006). This surface brightness is less than the limiting brightness at λ = 6 cm in the observations by Walter et al (1998), which were the basis for the identification of the SNR in Region # 11.…”

Section: The Expansion Of the H II Shells And Their Energy Budgetmentioning

confidence: 89%

The supergiant shell with triggered star formation in the dwarf irregular galaxy IC 2574: neutral and ionized gas kinematics

Egorov¹,

Lozinskaya²,

Моисеев³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We analyse the ionized gas kinematics in the star formation regions of the supergiant shell (SGS) of the IC 2574 galaxy using observations with the Fabry-Perot interferometer at the 6-m telescope of SAO RAS; the data of the THINGS survey are used to analyze the neutral gas kinematics in the area. We perform the 'derotation' of the Hα and H i data cubes and show its efficiency in kinematics analysis. We confirm the SGS expansion velocity 25 km s −1 obtained by Walter & Brinks (1999) and conclude that the SGS is located at the far side of the galactic disc plane. We determine the expansion velocities, kinematic ages, and the required mechanical energy input rates for four star formation complexes in the walls of the SGS; for the remaining ones we give the limiting values of the above parameters. A comparison with the age and energy input of the complexes' stellar population shows that sufficient energy is fed to all H ii regions except one. We discuss in detail the possible nature of this region and that of another one, which was believed to be an SNR according to radio observations. We measured the expansion velocity of the latter and confirm its identification as an old SNR. Our observations allowed us to identify a faint diffuse Hα emission inside the SGS which was never observed before.

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“…[31]) in the resonance approximation, when the particle giro-frequency is equal to the wave frequency in the system at rest with the particle motion along the average magnetic field. [42] within SM GCR, are shown in Fig. 1 in comparison with data.…”

Section: Standard Model For Galactic Cosmic Rays (Sm Gcr)mentioning

confidence: 89%

Transition from galactic to extragalactic cosmic rays

Aloisio

Berezinsky

Gazizov

2012

Astroparticle Physics

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a b s t r a c tThe study of the transition between galactic and extragalactic cosmic rays can shed more light on the end of the galactic cosmic rays spectrum and the beginning of the extragalactic one. Three models of transition are discussed: ankle, dip and mixed composition models. All these models describe the transition as an intersection of a steep galactic component with a flat extragalactic one. Severe bounds on these models are provided by the Standard Model of galactic cosmic rays according to which the maximum acceleration energy for Iron nuclei is of the order of E max Fe % 1 Â 10 17 eV. In the ankle model the transition is assumed at the ankle, a flat feature in the all particle spectrum which observationally starts at energy E a $ ð3 À 4Þ Â 10 18 eV. This model needs a new high energy galactic component with maximum energy about two orders of magnitude above that of the Standard Model. The origin of such component is discussed. As observations are concerned there are two signatures of the transition: change of energy spectra and mass composition. In all models a heavy galactic component is changed at the transition to a lighter or proton component. As a result the ankle model predicts a galactic Iron component at E < 5 Â 10 18 eV, while both HiRes and Auger data show that at ð2 À 5Þ Â 10 18 eV primaries are protons, or at least light nuclei. In the dip model the transition occurs at the second knee observed at energy ð4 À 7Þ Â 10 17 eV and is characterized by a sharp change of mass composition from galactic Iron to extragalactic protons. The ankle in this model appears automatically as a part of the e þ e À pair-production dip. The mixed composition model describes transition at E $ 3 Â 10 18 eV with mass composition changing from the galactic Iron to extragalactic mixed composition of different nuclei. In most mixed composition models the spectrum is proton-dominated and it better fits HiRes than Auger data. The latter show a steadily heavier mass composition with increasing energy, and we discuss the models which explain it.

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The theory of synchrotron emission from supernova remnants

Cited by 131 publications

References 48 publications

Radio-continuum study of MCSNR J0536–7038 (DEM L249)

Radio-continuum study of MCSNR J0536–7038 (DEM L249)

The supergiant shell with triggered star formation in the dwarf irregular galaxy IC 2574: neutral and ionized gas kinematics

Transition from galactic to extragalactic cosmic rays

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