The Galactic magnetic field as spectrograph for ultra-high energy cosmic rays

Kachelrieß, M.; Serpico, Pasquale Dario; Teshima, M.

doi:10.1016/j.astropartphys.2006.08.004

Cited by 74 publications

(87 citation statements)

References 35 publications

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“…The amplification of the UHECR flux by magnetic lensing was discussed previously in the context of the Galactic regular and turbulent field [23,24]. For instance, Ref.…”

Section: Discussionmentioning

confidence: 99%

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UHECR observations and lensing in the magnetic field of the Virgo cluster

Dolag

Kachelrieß

Semikoz

2009

J. Cosmol. Astropart. Phys.

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Abstract. We discuss how lensing by magnetic fields in galaxy clusters affects ultrahigh energy cosmic ray (UHECR) observations. As specific example, we use Virgo together with the cluster magnetic fields obtained earlier in a constrained simulation of structure formation including MHD processes. We find that, if M87 is the single source of UHECRs from Virgo, the emitted flux is strongly anisotropic in the most interesting energy range, (50-100) EeV, and differs from the average value by a factor five or more for a significant fraction of observers. Since magnetic lensing is energy dependent, the external energy spectrum as seen by different observers varies strongly too. These anisotropies are averaged out in the case that all active galactic nuclei in Virgo emit UHECRs. In both cases, the anisotropies of the emitted UHECR flux may introduce an important bias in the interpretation of UHECR data like, e.g., the determination of the source density n s and the source energy spectrum of UHECRs.

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“…The amplification of the UHECR flux by magnetic lensing was discussed previously in the context of the Galactic regular and turbulent field [23,24]. For instance, Ref.…”

Section: Discussionmentioning

confidence: 99%

“…For instance, Ref. [24] calculated exposure maps for three different models of the Galactic regular magnetic field and found also significant anisotropies at E = 40 EeV. The strength of the magnetic field close to the core of galaxy clusters is smaller by a factor 30-100 than in the Milky Way.…”

Section: Discussionmentioning

confidence: 99%

UHECR observations and lensing in the magnetic field of the Virgo cluster

Dolag

Kachelrieß

Semikoz

2009

J. Cosmol. Astropart. Phys.

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“…In this section we will restrict our discussion to how the extragalactic magnetic fields could modify the conclusions we reached in the previous section dedicated to the rectilinear regime. We will not discuss the propagation in the Galactic magnetic field but some details on the observations and constraints can be found in [106,108,108,110,105,107], analytical models of the magnetic fields in the Galaxy in [111,112,113] and studies on the propagation of UHECR and the expected consequences on their arrival directions in [111,112,114,113,115,116,117]. We will also not discuss in detail the impact of extragalactic magnetic fields on the expected anisotropies of the UHECR sky.…”

Section: Cosmic Magnetic Fieldsmentioning

confidence: 99%

Extragalactic propagation of ultrahigh energy cosmic-rays

Allard

2012

Astroparticle Physics

127

136

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In this paper we review the extragalactic propagation of ultrahigh energy cosmic-rays (UHECR). We present the different energy loss processes of protons and nuclei, and their expected influence on energy evolution of the UHECR spectrum and composition. We discuss the possible implications of the recent composition analyses provided by the Pierre Auger Observatory. The influence of extragalactic magnetic fields and possible departures from the rectilinear case are also mentioned as well as the production of secondary cosmogenic neutrinos and photons and the constraints their observation would imply for the UHECRs origin. Finally, we conclude by briefly discussing the relevance of a multi messenger approach for solving the mystery of UHECRs.

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“…It seems therefore possible to study the BSNR morphology to derive the geometry of the surrounding magnetic field, and thereby to investigate the microphysics of the particle acceleration processes that occur at the shock front. In this respect, BSNRs may be considered as a probe for structure of Galactic MF on scales of ∼10 pc, which is lower than the expected large scale variation of the field predicted by global models (Prouza & Šmída 2003;Kachelrieß et al 2007;Sun et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Constraints on the local interstellar magnetic field from non-thermal emission of SN1006

Bocchino

Orlando²,

Miceli³

et al. 2011

A&A

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Context. The synchrotron radio morphology of bilateral supernova remnants depends on the mechanisms of particle acceleration and on the viewing geometry. However, unlike X-ray and γ-ray morphologies, the radio emission does not depend on the cut-off region of the parent electron population, making it a simpler and more straightforward tool to investigate the physics of cosmic ray production in supernova remnants (SNRs). Aims. We will use the radio morphology to derive tight constraints on the direction of the local magnetic field and its gradient, and on the obliquity dependence of the electron injection efficiency. Methods. We perform a set of 3D MHD simulations describing the expansion of a spherical SNR through a magnetized medium with a non-uniform magnetic field. From the simulations, we derive non-thermal radio maps and compare them with observations of the SN1006 remnant. Results. We find that the radio morphology of SN1006 at 1 GHz is best-fitted by a model with quasi-parallel injection efficiency, a magnetic field aspect angle of 38 • ± 4 • with the line of sight, and a gradient of the field strength toward the galactic plane, higher then the expected variations of the large scale field of the Galaxy. Conclusions. We conclude that the radio limbs of SN1006 are polar caps that do not lie in the plane of sky. The study of the synchrotron radio emission of SNRs is of crucial importance to derive information on the galactic magnetic field in the vicinity of the remnants, and to gather more hints on the actual injection efficiency scenario.

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The Galactic magnetic field as spectrograph for ultra-high energy cosmic rays

Cited by 74 publications

References 35 publications

UHECR observations and lensing in the magnetic field of the Virgo cluster

UHECR observations and lensing in the magnetic field of the Virgo cluster

Extragalactic propagation of ultrahigh energy cosmic-rays

Constraints on the local interstellar magnetic field from non-thermal emission of SN1006

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