Ultrahigh Energy Cosmic Ray Nuclei from Extragalactic Pulsars and the effect of their Galactic counterparts

Fang, Ke; Kotera, Kumiko; Olinto, Angela V.

doi:10.48550/arxiv.1302.4482

Cited by 12 publications

(31 citation statements)

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“…In particular, we focus on magnetars in this work, and it is not obvious that these objects present such a distribution. Cosmic ray and neutrino productions from a cumulation of neutron star population following a (P, B) distribution can be found in [17,30]. We stress that the conclusions of these works (that focus on mildly magnetized pulsars) are not in contradiction with the present paper, because of the population distribution and the injection of a non-proton composition.…”

Section: Discussion Conclusionsupporting

confidence: 44%

“…[11][12][13] and has been resuscitated more recently by Refs. [14][15][16][17] are magnetized and fast-spinning neutron stars. These objects combine many advantages: their rotation speed endows them with a large energy reservoir (E rot ∼ 2 × 10 52 erg I 45 P −2 −3 , with I the star inertial momentum and P its spin period 1 , for an isolated new-born pulsar spinning close to the disruption limit), and their population density ( ṅs ∼ 10 −4 Mpc −3 yr −1 [18]) is high enough to allow a comfortable total energy budget.…”

Section: Introductionmentioning

confidence: 99%

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IceCube constraints on fast-spinning pulsars as high-energy neutrino sources

Fang

Kotera

Murase

et al. 2016

J. Cosmol. Astropart. Phys.

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Abstract. Relativistic winds of fast-spinning pulsars have been proposed as a potential site for cosmic-ray acceleration from very high energies (VHE) to ultrahigh energies (UHE). We re-examine conditions for high-energy neutrino production, considering the interaction of accelerated particles with baryons of the expanding supernova ejecta and the radiation fields in the wind nebula. We make use of the current IceCube sensitivity in diffusive highenergy neutrino background, in order to constrain the parameter space of the most extreme neutron stars as sources of VHE and UHE cosmic rays. We demonstrate that the current non-observation of 10 18 eV neutrinos put stringent constraints on the pulsar scenario. For a given model, birthrates, ejecta mass and acceleration efficiency of the magnetar sources can be constrained. When we assume a proton cosmic ray composition and spherical supernovae ejecta, we find that the IceCube limits almost exclude their significant contribution to the observed UHE cosmic-ray flux. Furthermore, we consider scenarios where a fraction of cosmic rays can escape from jet-like structures piercing the ejecta, without significant interactions. Such scenarios would enable the production of UHE cosmic rays and help remove the tension between their EeV neutrino production and the observational data.

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Section: Discussion Conclusionsupporting

confidence: 44%

Section: Introductionmentioning

confidence: 99%

IceCube constraints on fast-spinning pulsars as high-energy neutrino sources

Fang

Kotera

Murase

et al. 2016

J. Cosmol. Astropart. Phys.

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“…From the theoretical point of view the hard injection spectrum is interesting in that it suggests that acceleration mechanisms such as those that take place in the magnetosphere of rapidly rotating neutron stars [41,42,43,44] or in the accretion discs around massive black holes [57] may play a role. Moreover, it is fair to assume that the environment around a neutron star may be polluted with heavy nuclei, provided such nuclei can be stripped off the surface of the star.…”

Section: Discussionmentioning

confidence: 99%

“…1, the maximum acceleration energy for protons is E p max = 5 × 10 18 eV and for nuclei E A max = Z × E p max . The hard injection spectra required to fit the Auger data are reminiscent of models of the origin of UHECRs associated to acceleration in rapidly rotating neutron stars [41,42,43,44], although hard spectra are a more general characteristic of acceleration scenarios where regular electric fields are available (e.g. unipolar induction and reconnection).…”

Section: Spectra Of Uhecrs Propagating Through the Cmb And Eblmentioning

confidence: 99%

“…The combination of hard injection spectrum and low E max allows us to reach a satisfactory simultaneous agreement with both the spectrum at E > 5 × 10 18 eV and the chemical composition, though with a slight tendency toward a too heavy composition at the highest energies, thereby confirming a result previously presented in Refs. [8,44].…”

Section: Spectra Of Uhecrs Propagating Through the Cmb And Eblmentioning

confidence: 99%

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Ultra high energy cosmic rays: implications of Auger data for source spectra and chemical composition

Aloisio

Berezinsky

Blasi

2014

J. Cosmol. Astropart. Phys.

147

184

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Abstract. We use a kinetic-equation approach to describe the propagation of ultra high energy cosmic ray protons and nuclei and calculate the expected spectra and mass composition at the Earth for different assumptions on the source injection spectra and chemical abundances. When compared with the spectrum, the elongation rate X max (E) and dispersion σ(X max ) as observed with the Pierre Auger Observatory, several important consequences can be drawn: a) the injection spectra of nuclei must be very hard, ∼ E −γ with γ ∼ 1 − 1.6; b) the maximum energy of nuclei of charge Z in the sources must be ∼ 5Z × 10 18 eV, thereby not requiring acceleration to extremely high energies; c) the fit to the Auger spectrum can be obtained only at the price of adding an ad hoc light extragalactic component with a steep injection spectrum (∼ E −2.7 ). In this sense, at the ankle (E A ≈ 5 × 10 18 eV) all the components are of extragalactic origin, thereby suggesting that the transition from Galactic to extragalactic cosmic rays occurs below the ankle. Interestingly, the additional light extragalactic component postulated above compares well, in terms of spectrum and normalization, with the one recently measured by KASCADE-Grande.

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UHECR composition models

Taylor¹

2014

Astroparticle Physics

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In light of the increasingly heavy UHECR composition at the highest energies, as observed by the Pierre Auger Observatory, the implications of these results on the actual source composition and spectra are investigated. Depending on the maximum energy of the particles accelerated, sources producing hard spectra and/or containing a considerably enhanced heavy component appear a necessary requirement. Consideration is made of two archetypal models compatible with these results. The secondary signatures expected , following the propagation of the nuclear species from source to Earth, are determined for these two example cases. Finally, the effect introduced by the presence of nG extragalactic magnetic fields in collaboration with a large (80 Mpc) distance to the nearest source is discussed.

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Ultrahigh Energy Cosmic Ray Nuclei from Extragalactic Pulsars and the effect of their Galactic counterparts

Cited by 12 publications

References 0 publications

IceCube constraints on fast-spinning pulsars as high-energy neutrino sources

IceCube constraints on fast-spinning pulsars as high-energy neutrino sources

Ultra high energy cosmic rays: implications of Auger data for source spectra and chemical composition

UHECR composition models

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