Ultrahigh energy cosmic ray acceleration in newly born magnetars and their associated gravitational wave signatures

Kotera, Kumiko

doi:10.1103/physrevd.84.023002

Cited by 27 publications

(34 citation statements)

References 76 publications

(139 reference statements)

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“…, (18) where S and S ′ denote UHECR sources and sources randomly distributed following selection effects of the catalog of the source candidates. S ′ is isotropically distributed in the entire sky in this study because of the correction of selection effects (see Section 2.4).…”

Section: Statistical Quantitiesmentioning

confidence: 99%

“…In either case, the maximum energy of 10 20 eV can only be achieved in extreme environments [1]. Prominent source candidates suggested so far include active galactic nuclei (AGN) [2,3,4,5,6,7,8,9,10], gamma-ray bursts (GRBs) [11,12,13,14], neutron stars or magnetars [15,16,17,18] and clusters of galaxies [19,20,21]. If UHECRs with energies above ∼ 6 × 10 19 eV are mainly protons, their propagation distance should be limited by interactions with cosmic microwave background (CMB) photons [22,23,24,25,26], the so-called Greisen-Zatsepin-Kuz'min (GZK) mechanism, so that they are observable only from sources sufficiently nearby (typically 200 Mpc).…”

Section: Introductionmentioning

confidence: 99%

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Propagation of ultra-high-energy cosmic ray nuclei in cosmic magnetic fields and implications for anisotropy measurements

Takami

Inoue

Yamamoto

2012

Astroparticle Physics

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Recent results from the Pierre Auger Observatory (PAO) indicate that the composition of ultra-high-energy cosmic rays (UHECRs) with energies above 10 19 eV may be dominated by heavy nuclei. An important question is whether the distribution of arrival directions for such UHECR nuclei can exhibit observable anisotropy or positional correlations with their astrophysical source objects despite the expected strong deflections by intervening magnetic fields. For this purpose, we have simulated the propagation of UHECR nuclei including models for both the extragalactic magnetic field (EGMF) and the Galactic magnetic field (GMF). We find that the GMF is particularly crucial for suppressing the anisotropy as well as source correlations. Assuming that only iron nuclei are injected steadily from sources with equal luminosity and spatially distributed according to the observed large scale structure in the local Universe, at the number of events published by the PAO so far (69 events above 5.5 × 10 19 eV), the arrival distribution of UHECRs would be consistent with no auto-correlation at 95% confidence if the mean number density of UHECR sources n s 10 −6 Mpc −3 , and consistent with no cross-correlation with sources within 95% errors for n s 10 −5 Mpc −3 . On the other hand, with 1000 events above 5.5 × 10 19 eV in the whole sky, next generation experiments can reveal auto-correlation with more than 99% probability even for n s 10 −3 Mpc −3 , and cross-correlation with sources with more than 99% probability for n s 10 −4 Mpc −3 . In addition, we find that the contribution of Centaurus A is required to reproduce the currently observed UHECR excess in the Centaurus region. Secondary protons generated by photodisintegration of primary heavy nuclei during propagation play a crucial role in all cases, and the resulting anisotropy at small angular scales should provide a strong hint of the source location if the maximum energies of the heavy nuclei are sufficiently high.

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Section: Statistical Quantitiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Propagation of ultra-high-energy cosmic ray nuclei in cosmic magnetic fields and implications for anisotropy measurements

Takami

Inoue

Yamamoto

2012

Astroparticle Physics

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“…[37][38][39] have also suggested that jetted TDEs may lead to hard spectra.Even if hard spectra production were achieved at each source, it is likely that the overall diffuse UHECR spectrum softens through the integration over the population of sources. Indeed, sources with milder characteristics, which will produce lower-energy particles, are more numerous, and the distribution of their parameters will naturally soften the spectrum [40,41]. A hard spectrum production is thus difficult to justify from a source population point of view.The suppression of the low-energy part of the UHECR spectrum due to the diffusion of low-energy particles in extragalactic magnetic fields, the magnetic horizon effect, has been proposed as a solution to this problem [42,43].…”

mentioning

confidence: 99%

Cosmogenic photon and neutrino fluxes in the Auger era

Batista

Almeida

Lago

et al. 2019

J. Cosmol. Astropart. Phys.

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145

209

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The interaction of ultra-high-energy cosmic rays (UHECRs) with pervasive photon fields generates associated cosmogenic fluxes of neutrinos and photons due to photohadronic and photonuclear processes taking place in the intergalactic medium. We perform a fit of the UHECR spectrum and composition measured by the Pierre Auger Observatory for four source emissivity scenarios: power-law redshift dependence with one free parameter, active galactic nuclei, gamma-ray bursts, and star formation history. We show that negative source emissivity evolution is favoured if we treat the source evolution as a free parameter. In all cases, the best fit is obtained for relatively hard spectral indices and low maximal rigidities, for compositions at injection dominated by intermediate nuclei (nitrogen and silicon groups). In light of these results, we calculate the associated fluxes of neutrinos and photons. Finally, we discuss the prospects for the future generation of high-energy neutrino and gamma-ray observatories to constrain the sources of UHECRs. understood, the prospects for ultra-high-energy cosmic-ray astronomy are unclear (see e.g. Refs. [6][7][8]).The so-called dip model [9, 10] postulates a purely protonic composition for the UHECR flux and was once the prevalent paradigm. However, many pure proton models have been disfavoured due to the fact that they overproduce the diffuse gamma-ray background (DGRB) [11][12][13][14][15] and/or violate neutrino limits [16][17][18]. Because protons tend to contribute to the overall cosmogenic fluxes considerably more than other nuclei, even in a mixed-composition scenario it is possible to set limits on the total fraction of protons arriving at Earth based on the associated cosmogenic fluxes [19,20]. In recent years, much effort has been put into this kind of study [21][22][23].Recently the Pierre Auger Collaboration has performed a combined spectrum-composition fit [24]. A number of simplified assumptions are made in this work, namely that the sources are uniformly distributed within the comoving volume and that only five nuclear species are emitted (H, He, N, Si, and Fe), being these five species a representative sample that can approximately describe reality. The extragalactic magnetic field is assumed to be null. It was also attempted to account for theoretical uncertainties related to the modelling of propagation and cross check results of two simulations codes, photonuclear cross sections, and models of the EBL.The results of the Auger fit are rather surprising, pointing to a "hard-spectrum problem", favouring low spectral indices (α 1), and posing challenges to the current acceleration paradigm. The situation can be alleviated by making a distinction between the spectrum of the accelerated particles (α acc ) and the one of the escaping particles (α esc ), since interactions with the gas and photons surrounding a source and the local magnetic fields can drastically change the spectral shape. In the following discussion, unless otherwise stated, we will refer to the escape spectr...

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“…Despite decades of observations and modelling (see e.g. Kotera 2011;Abbasi et al 2012 andAloisio 2018 for recent reviews) the underlying source remains uncertain.…”

Section: Ultra-high Energy Cosmic Raysmentioning

confidence: 99%

A quark nova in the wake of a core-collapse supernova: a unifying model for long duration gamma-ray bursts and fast radio bursts

Ouyed

Leahy

Koning

2020

Res. Astron. Astrophys.

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By appealing to a Quark-Nova (QN; the explosive transition of a neutron star to a quark star) in the wake of a core-collapse Supernova explosion of a massive star, we develop a unified model for long duration Gamma-ray Bursts (LGRBs) and Fast Radio Bursts (FRBs). The time delay (years to decades) between the SN and the QN and, the fragmented nature (i.e. millions of chunks) of the relativistic QN ejecta are key to yielding a robust LGRB engine. In our model, a LGRB light-curve exhibits the interaction of the fragmented QN ejecta with a turbulent (i.e. filamentary and magnetically saturated) SN ejecta which is shaped by its interaction with an underlying pulsar wind nebula (PWN). The afterglow is due to the interaction of the QN chunks, exiting the SN ejecta, with the surrounding medium. Our model can fit BAT/XRT prompt and afterglow light-curves, simultaneously with their spectra, thus yielding the observed properties of LGRBs (e.g. the Band function and the X-ray flares). We find that the peak luminosity-peak photon energy relationship (i.e. the Yonetoku law), and the isotropic energy-peak photon energy relationship (i.e. the Amati law) are not fundamental but phenomenological. FRBs in our model result from coherent synchrotron emission (CSE) when the QN chunks interact with non-turbulent weakly magnetized PWN-SN ejecta, where conditions are prone to the Weibel instability. Magnetic field amplification induced by the Weibel instability in the shocked chunk frame sets the bunching length for electrons and pairs to radiate coherently. The resulting emission frequency, luminosity, duration and dispersion measure (DM) in our model are consistent with FRB data. We find a natural unification of high-energy burst phenomena from FRBs to LGRBs including X-ray Flashes (XRFs) and X-ray rich GRBs (XRR-GRBs) as well as Super-Luminous SNe (SLSNe). We find a possible connection between Ultra-High Energy Cosmic Rays and FRBs and propose that a QN following a binary neutron star merger can yield a short GRB (SGRB) with fits to BAT/XRT light-curves.

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Ultrahigh energy cosmic ray acceleration in newly born magnetars and their associated gravitational wave signatures

Cited by 27 publications

References 76 publications

Propagation of ultra-high-energy cosmic ray nuclei in cosmic magnetic fields and implications for anisotropy measurements

Propagation of ultra-high-energy cosmic ray nuclei in cosmic magnetic fields and implications for anisotropy measurements

Cosmogenic photon and neutrino fluxes in the Auger era

A quark nova in the wake of a core-collapse supernova: a unifying model for long duration gamma-ray bursts and fast radio bursts

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