Cosmic rays escaping from Galactic starburst-driven superbubbles

Zhang, Zhaowei; Murase, Kohta; Mészáros, P.

doi:10.1093/mnras/staa022

Cited by 9 publications

(7 citation statements)

References 60 publications

(80 reference statements)

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“…5 and it is compared with observations by Fermi-LAT 29 , IceCube 30 , IceTop 34 , Tunka 31,32 and Kascade-Grande 33 . While the total gamma-ray flux from SB-driven wind bubbles contributes approximately to ∼ 5 − 10% of the Fermi-LAT data, leaving enough room for SBNi 35,36,37,38 and AGNi 16,39 , the total neutrino flux and the associated CR flux could provide a sizeable contribution and possibly saturate part of the observed spectra 14,40 .…”

Section: Discussionmentioning

confidence: 99%

Particle acceleration in galactic wind bubbles

Peretti¹

2022

Preprint

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Winds are ubiquitous in galaxies and often feature bubble structures. These wind bubbles are characterized by an external forward shock expanding in the surrounding medium and a wind termination shock separating the cool and fast wind from the hot shocked wind. While the forward shock could not be able to accelerate particles efficiently for a long time, at the wind termination shock the necessary conditions for efficient acceleration may be present. We develop a model for particle acceleration at the termination shock of such bubbles analysing the consequences of different possible engines powering the wind. We finally explore the multimessenger potential of galactic winds in terms of escaping cosmic rays and high-energy gamma rays and neutrinos produced through hadronic interactions.

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Section: Discussionmentioning

confidence: 99%

Particle acceleration in galactic wind bubbles

Peretti¹

2022

Preprint

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“…A new solution for the 1D diffusion equation with losses proportional to the concentration was derived, see Equations ( 13) and (14).…”

Section: Conclusion Diffusion With Stationary Statementioning

confidence: 99%

“…analysis of the generalized Kompaneets' equations adapted to expansion in various external density profiles and coupled with escaping CRs [14], production of γ-ray radiation in the interactions between cosmic rays and interstellar gas in the Orion-Eridanus SB [15] and acceleration of particles and non-linear feedback [16]. Another point for research is the excess in γ-rays observed by the Fermi Large Area Telescope at the centre of the Galaxy, which can be explained by annihilating dark matter, [17].…”

Section: Introductionmentioning

confidence: 99%

Transport in Astrophysics: III. Diffusion from the Galactic Plane

Zaninetti¹

2023

IJAA

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New solutions, for the stationary and temporary states, are derived for the 1D diffusion of cosmic rays in the presence of losses. The new results are applied to the latitude profile of radiation emitted above the galactic plane. Percolation theory for a spiral galaxy coupled with the evolution of the super-bubbles allows building a model for the radiation of a spiral galaxy as seen face on. The annulus of radiation of our galaxy is also simulated and the excess of radiation observed at the centre of our galaxy is explained by the sine law which arises in the theory of the image.

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“…Superbubbles may accelerate cosmic rays up to PeV energies or beyond via multiple shocks and turbulence (Bykov & Fleishman 1992;Klepach et al 2000). It has been shown that cosmic rays escaping from star clusters or superbubbles may explain cosmic rays above the knee energy (Murase & Fukugita 2019;Zhang et al 2020). The Cygnus region has also been of much interest as the promising source of high-energy neutrinos (e.g., Anchordoqui et al 2007;Beacom & Kistler 2007;Halzen & O Murchadha 2007;Halzen et al 2017).…”

Section: Contribution Of Discrete Sources To Sub-pev Gamma Rays and N...mentioning

confidence: 99%

Multi-messenger Implications of Sub-PeV Diffuse Galactic Gamma-Ray Emission

Fang,

Murase

2021

Preprint

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The diffuse Galactic gamma-ray flux between 0.1 and 1 PeV has recently been measured by the Tibet ASγ Collaboration. The flux and spectrum are consistent with the decay of neutral pions from hadronuclear interactions between Galactic cosmic rays and the interstellar medium (ISM). We derive the flux of the Galactic diffuse neutrino emission from the same interaction process that produces the gamma rays. Our calculation accounts for the effect of gamma-ray attenuation inside the Milky Way and uncertainties due to the spectrum and distribution of cosmic rays, gas density, and infrared emission of the ISM. We find that the contribution from the Galactic plane to the all-sky neutrino flux is 5 − 10% around 100 TeV. The Galactic and extragalactic neutrino intensities are comparable in the Galactic plane region. Our results are consistent with the upper limit reported by the IceCube and ANTARES Collaborations, and predict that next-generation neutrino experiments may observe the Galactic component. We also show that the Tibet ASγ data imply either an additional component in the cosmic-ray nucleon spectrum or contribution from discrete sources, including Pevatrons such as superbubbles and hypernova remnants, and PeV electron accelerators. Future multi-messenger observations between 1 TeV and 1 PeV are crucial to decomposing the origin of sub-PeV gamma rays.

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Cosmic rays escaping from Galactic starburst-driven superbubbles

Cited by 9 publications

References 60 publications

Particle acceleration in galactic wind bubbles

Particle acceleration in galactic wind bubbles

Transport in Astrophysics: III. Diffusion from the Galactic Plane

Multi-messenger Implications of Sub-PeV Diffuse Galactic Gamma-Ray Emission

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