Gamma-ray puzzle in Cygnus X: Implications for high-energy neutrinos

Yoast-Hull, Tova M.; Gallagher, John S.; Halzen, F.; Kheirandish, Ali; Zweibel, Ellen G.

doi:10.1103/physrevd.96.043011

Cited by 21 publications

(17 citation statements)

References 62 publications

(107 reference statements)

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“…High-energy neutrinos produced by inelastic nuclei collisions in the Cygnus X region may have a large enough flux to be detected with the IceCube Observatory, as estimated by Yoast-Hull et al (2017) using a single-zone model of CR interactions with the molecular gas. The planned observations of the Cygnus region with the high sensitivity and good angular resolution Cherenkov Telescope Array have the potential to provide imaging and spectra of the region between a few tens of GeV up to ∼ 100 TeV (Weinstein et al 2015).…”

Section: Cosmic Rays In Superbubblesmentioning

confidence: 99%

Cosmic Ray Production in Supernovae

et al. 2018

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We give a brief review of the origin and acceleration of cosmic rays (CRs), emphasizing the production of CRs at different stages of supernova evolution by the first-order Fermi shock acceleration mechanism. We suggest that supernovae with trans-relativistic outflows, despite being rather rare, may accelerate CRs to energies above 10 18 eV over the first year of their evolution. Supernovae in young compact clusters of massive stars, and interaction powered superluminous supernovae, may accelerate CRs well above the PeV regime. We discuss the acceleration of the bulk of the galactic CRs in isolated supernova remnants and re-acceleration of escaped CRs by the multiple shocks present in superbubbles produced by associations of OB stars. The effects of magnetic field amplification by CR driven instabilities, as well as superdiffusive CR transport, are discussed for nonthermal radiation produced by nonlinear shocks of all speeds including trans-relativistic ones.

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Section: Cosmic Rays In Superbubblesmentioning

confidence: 99%

Cosmic Ray Production in Supernovae

et al. 2018

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“…The influence of the models is evident as Tova et al [36] suggest a neutrino spectrum from Cygnus X which is most likely not detectable, whereas the model from this work coincides with the limit of IceCube. Additionally, in Figure 8…”

Section: Cosmic Raysmentioning

confidence: 52%

Cosmic Ray Cradles in the Galaxy

Guenduez¹,

Tjus²,

Eichmann³

et al. 2018

Cosmic Rays

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The search for the origin of high-energy cosmic rays has made significant progress in the past decade. By including multi-messenger methods, the general picture of the presence of a galactic component at low energies and an extragalactic one at the highest energies has been strengthened. Yet, unambiguous proof of the exact origins of cosmic rays is still missing. This chapter will review localized regions in the galaxy, which, due to their high nonthermal emission, are likely cosmic ray cradles. What we can learn from combining theoretical modeling with multi-messenger observations of regions like the Cygnus X complex, the Eta Carinae, and the Galactic Center region will be discussed. How the investigation of such localized regions in the Milky Way will help to resolve the more than 100-year-old question: what is the origin of cosmic rays? will be reviewed.

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“…Secondary particle interactions can produce observable emissions not only in interacting galaxy systems but also in star-forming and/or starburst galaxies, where supernovae can accelerate high-energy CRs and trigger subsequent particle interactions. Previous studies incorporating π 0 decays, bremsstrahlung, inverse Compton and synchrotron emissions have shown that CR interactions can be used to explain the gamma-ray observations of the starburst galaxy M82 (Yoast-Hull et al 2013), the Cygnus X region (Yoast-Hull et al 2017b) and the ultra-luminous infrared galaxy Arp 220 (Yoast-Hull et al 2017a). Interestingly, for Arp 220 we can estimate the CR luminosity density from a galaxy merger scenario in the central molecular zone as L cr,merger 1 2 p M g v 2 s R vs −1 ≈ 9.87 × 10 43 vs 500km s −1 3 erg s −1 , using the gas mass M g = 6 × 10 8 M (Sakamoto et al 2008) and R = 70 pc (Downes & Eckart 2007), which is roughly twice as much as the best-fitting supernova CR luminosity Yoast-Hull et al (2015), L cr,SNe E cr,SN R SN ≈ 4.76 × 10 43 erg s −1 , for a typical CR energy injected by supernovae of E cr,SN ≈ 10 50 erg and a supernova rate R SN ≈ 15 yr −1 .…”

Section: Summary and Discussionmentioning

confidence: 99%

Secondary Radio and X-Ray Emissions from Galaxy Mergers

Yuan

Murase

Mészáros

2019

ApJ

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Shocks arising in galaxy mergers could accelerate cosmic-ray (CR) ions to TeV-PeV energies. While propagating in the intergalactic medium, these CRs can produce high-energy neutrinos, electronpositron pairs and gamma-rays. In the presence of intergalactic magnetic fields, the secondary pairs will radiate observable emissions through synchrotron radiation and inverse Compton scattering. In this paper, we demonstrate that these emissions can explain the radio and X-ray fluxes of merging galaxies such as NGC 660 and NGC 3256. Using our model in combination with the observations, we can constrain the gas mass, shock velocity, magnetic field and the CR spectral index s of these systems. For NGC 660 a single-zone model with a spectral index 2.1 ∼ < s ∼ < 2.2 is able to reproduce simultaneously the radio and X-ray observations, while a simple one-zone scenario with s ∼ 2 can describe the radio and a large fraction of X-ray observations of NGC 3256. Our work provides a useful approach for studying the dynamics and physical parameters of galaxy mergers, which can play an important part in future multi-messenger studies of similar and related extragalactic sources.

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Gamma-ray puzzle in Cygnus X: Implications for high-energy neutrinos

Cited by 21 publications

References 62 publications

Cosmic Ray Production in Supernovae

Cosmic Ray Production in Supernovae

Cosmic Ray Cradles in the Galaxy

Secondary Radio and X-Ray Emissions from Galaxy Mergers

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