Probing Lorentz invariance at EeV energy

Moharana, Reetanjali; Gupta, Nayantara

doi:10.1088/1475-7516/2009/08/005

Cited by 5 publications

(4 citation statements)

References 44 publications

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“…where l c is the coherence length (Stanev 1997;Moharana & Gupta 2009) and E p,th = 57 EeV is the energy threshold of TA experiment. Due to the strength of extragalactic (B EG 1 nG) and galactic (B G 4 µG) magnetic fields, UHECRs are deflected (ψ EG 5 • and ψ G 3.8 • ) between the true direction to the source, and the observed arrival direction, respectively.…”

Section: Hillas Condition and Deflexionsmentioning

confidence: 99%

TeV γ-ray fluxes from the long campaigns on Mrk 421 as constraints on the emission of TeV–PeV neutrinos and UHECRs

Fraija

Marinelli

2015

Astroparticle Physics

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a b s t r a c tLong TeV c-ray campaigns have been carried out to study the spectrum, variability and duty cycle of the BL Lac object Markarian 421. These campaigns have given some evidence of the presence of protons in the jet: (i) Its spectral energy distribution which shows two main peaks; one at low energies ($1 keV) and the other at high energies (hundreds of GeV), has been described by using synchrotron proton blazar model. (ii) The study of the variability at GeV c-rays and X-rays has indicated no significant correlation. (iii) TeV c-ray detections without activity in X-rays, called ''orphan flares'' have been observed in this object.Recently, The Telescope Array Collaboration reported the arrival of 72 ultra-high-energy cosmic rays with some of them possibly related to the direction of Markarian 421. The IceCube Collaboration reported the detection of 37 extraterrestrial neutrinos in the TeV-PeV energy range collected during three consecutive years. In particular, no neutrino track events were associated with this source. In this paper, we consider the proton-photon interactions to correlate the TeV c-ray fluxes reported by long campaigns with the neutrino and ultra-high-energy cosmic ray observations around this blazar. Considering the results reported by The IceCube and Telescope Array Collaborations, we found that only from $25% to 70% of TeV fluxes described with a power law function with exponential cutoff can come from the proton-photon interactions.

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Section: Hillas Condition and Deflexionsmentioning

confidence: 99%

TeV γ-ray fluxes from the long campaigns on Mrk 421 as constraints on the emission of TeV–PeV neutrinos and UHECRs

Fraija

Marinelli

2015

Astroparticle Physics

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“…(6) to obtain the expression for fπ(Ep,j). A simplified expression was given by Waxman & Bahcall (1997), whereas a more general expression involves the spectral indices γ1 and γ2 (Gupta & Zhang 2007, Moharana & Gupta 2012.…”

Section: P γ Interactions As a Plausible Source Of The Positron Excessmentioning

confidence: 99%

“…In terms of the proton energy Ep and the break energy in the proton spectrum E pb , which appears due to the break in the low energy photon spectrum at ǫ br it is (Gupta & Zhang 2007, Moharana & Gupta 2012…”

Section: P γ Interactions As a Plausible Source Of The Positron Excessmentioning

confidence: 99%

pγ interactions in Galactic jets as a plausible origin of the positron excess

Gupta

Torres

2014

Monthly Notices of the Royal Astronomical Society

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“…magnetic fields. Here L EG corresponds to the average path of extragalactic charged particle going through our Galaxy (20 kpc), l c is the coherence length (Stanev 1997;Moharana & Gupta 2009) and E p,th = 57 EeV is the threshold energy of the TA experiment.…”

Section: Uhe Cosmic Rays Phenomenologymentioning

confidence: 99%

The Hadronic Picture of the Radiogalaxy M87

Marinelli,

Fraija,

Patricelli

2014

Preprint

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Very high energy gamma-ray emission of Fanaroff-Riley I objects is not univocally explained by a single emission model. Leptonic models with one and multi-zone emission regions, occurring in the jet of these objects, are usually used to describe the broadband spectral energy distribution. A correlation between the X-ray and TeV emission is naturally expected within leptonic models whereas a lack of correlation between these two observables represents a challenge and favors the hadronic scenarios. This is the case of M87 as we show here by analyzing its TeV and X-ray emission recorded in the last decade. Furthermore, we point out that the spectra obtained by MAGIC, H.E.S.S. and VERITAS telescopes cannot be described with the same leptonic model introduced by the Fermi-LAT collaboration. We introduce hadronic scenarios to explain the TeV gamma-ray fluxes of this radiogalaxy as products of Fermi-accelarated protons interacting with seed photons in the jet or thermal particles in the giant lobes. By fitting this part of spectral energy distribution as pion decay products, we obtain the expected neutrino counterpart and the luminosity of accelerating protons in the jet and/or lobes. With the expected neutrino fluxes we investigate, through Monte Carlo simulations, the possibility to see the signal from M87 with a Km 3 neutrino telescope, and compare the results with what has been seen by IceCube experiment up to now. Finally we constrain the features of giant lobes through the observations performed at ultra high energies by TA experiment.

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Probing Lorentz invariance at EeV energy

Cited by 5 publications

References 44 publications

TeV γ-ray fluxes from the long campaigns on Mrk 421 as constraints on the emission of TeV–PeV neutrinos and UHECRs

TeV γ-ray fluxes from the long campaigns on Mrk 421 as constraints on the emission of TeV–PeV neutrinos and UHECRs

pγ interactions in Galactic jets as a plausible origin of the positron excess

The Hadronic Picture of the Radiogalaxy M87

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