The Galactic distribution of SNRs

Green, David A.

doi:10.1017/s1743921313009459

Cited by 9 publications

(8 citation statements)

References 22 publications

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“…2.2 below), and concentrated in the Galactic disc. For example, the distribution of supernova remnants as described in Green (2014), with radial profile n(r) = (r/R ) 0.7 exp[−3.5(r − R )/R ], as employed in the study Giacinti et al (2014), will give an identical qualitative picture, and a very similar quantitative one. With such generic assumptions it is also not important whether the sources are transient or not.…”

Section: Source Distributionmentioning

confidence: 99%

A signature of EeV protons of Galactic origin

Tinyakov

Urban

Ivanov

et al. 2016

Mon. Not. R. Astron. Soc.

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We investigate signatures that would be produced in the spectrum and sky distribution of UHECR by a population of the Galactic sources of high-energy protons in the energy range around 1 EeV, i.e., around the diffusive-to-ballistic transition. In this regime, the CR flux has to be calculated numerically. We employ the approach that consists in backtracking anti-protons from Earth through the Galaxy and integrating the source emissivity along the trajectory. This approach makes evident two generic features of the transition region: sharp increase of the total flux as the energy decreases across the transition region, and its strong anisotropy (appearance of a bright compact spot) all the way until the onset of the diffusive regime. We then discuss and compare several methods to experimentally detect or constrain these features. We find that a few percent admixture of the Galactic protons can in principle be detected by the current UHECR experiments.

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Section: Source Distributionmentioning

confidence: 99%

A signature of EeV protons of Galactic origin

Tinyakov

Urban

Ivanov

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The sample of SNRs in the Galaxy is not really complete, at least in the sense that all SNRs of certain intrinsic properties in the Galaxy have been discovered. Green [79] estimates that the radio sample is approximately complete to a surface brightness limit of 10 −20 Watts m −2 Hz −1 sr −1 . There are 68 SNRs brighter than this limit, but Green notes that a selection bias still exists.…”

Section: The Galaxymentioning

confidence: 99%

“…If all SNRs had the same radio luminosity, then Σ ∝ D −2 . Errors arise not only from the fact that SNRs from identical SNe evolving in different ISM may have different radio luminosities at the same diameter, but also from sample completeness biases, and in some cases, the way in which the power law index is derived from the observational data [79].…”

Section: Radio Surface Brightness -Diameter Relationship σ -Dmentioning

confidence: 99%

“…Clark & Caswell [142] in an early analysis of the Galactic sample derived a value of about -3, similar to the value Mathewson & Clark [5] had found for LMC SNRs. Case & Bhattacharya [144] found a value 2.64 for a sample of 37 SNRs, which included Cas A, although their analysis approach has been criticized by Green [79]. Pavlović et al [145,140], who attempt to account for the distance uncertainties for individual objects, find steeper exponents of order -5.…”

Section: Radio Surface Brightness -Diameter Relationship σ -Dmentioning

confidence: 99%

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Galactic and Extragalactic Samples of Supernova Remnants: How They Are Identified and What They Tell Us

Long

2017

Handbook of Supernovae

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Supernova remnants (SNRs) arise from the interaction between the ejecta of a supernova (SN) explosion and the surrounding circumstellar and interstellar medium. Some SNRs, mostly nearby SNRs, can be studied in great detail. However, to understand SNRs as a whole, large samples of SNRs must be assembled and studied. Here, we describe the radio, optical, and X-ray techniques which have been used to identify and characterize almost 300 Galactic SNRs and more than 1200 extragalactic SNRs. We then discuss which types of SNRs are being found and which are not. We examine the degree to which the luminosity functions, surface-brightness distributions and multi-wavelength comparisons of the samples can be interpreted to determine the class properties of SNRs and describe efforts to establish the type of SN explosion associated with a SNR. We conclude that in order to better understand the class properties of SNRs, it is more important to study (and obtain additional data on) the SNRs in galaxies with extant samples at multiple wavelength bands than it is to obtain samples of SNRs in other galaxies.

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“…The origin of high energy cosmic rays (CR) remains uncertain, nevertheless supernova remnants are being promoted as the most promising candidates for providing the CR flux up to PeV energies measured at Earth (Fermi, 1949;Blandford and Ostriker, 1978;Hillas, 2005). Due to shock front acceleration in the surrounding dust cloud, charged particles are able to reach energies up to that order.…”

Section: Introductionmentioning

confidence: 99%

Gamma-ray emitting supernova remnants as the origin of Galactic cosmic rays

et al. 2015

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Abstract. It is generally believed that the cosmic ray spectrum below the knee is of Galactic origin, although the exact sources making up the entire cosmic ray energy budget are still unknown. Including effects of magnetic amplification, Supernova Remnants (SNR) could be capable of accelerating cosmic rays up to a few PeV and they represent the only source class with a sufficient non-thermal energy budget to explain the cosmic ray spectrum up to the knee. Now, gamma-ray measurements of SNRs for the first time allow to derive the cosmic ray spectrum at the source, giving us a first idea of the concrete, possible individual contributions to the total cosmic ray spectrum. In this contribution, we use these features as input parameters for propagating cosmic rays from its origin to Earth using GALPROP in order to investigate if these supernova remnants reproduce the cosmic ray spectrum and if supernova remnants in general can be responsible for the observed energy budget.

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The Galactic distribution of SNRs

Cited by 9 publications

References 22 publications

A signature of EeV protons of Galactic origin

A signature of EeV protons of Galactic origin

Galactic and Extragalactic Samples of Supernova Remnants: How They Are Identified and What They Tell Us

Gamma-ray emitting supernova remnants as the origin of Galactic cosmic rays

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