Particle acceleration and the origin of gamma-ray emission from Fermi bubbles

D. O. Chernyshov; K. S. Cheng; V. A. Dogiel; C. M. Ko; W. H. Ip; Y. Wang

doi:10.7529/ICRC2011/V07/0589

Particle acceleration and the origin of gamma-ray emission from Fermi bubbles

D. O. Chernyshov, K. S. Cheng, V. A. Dogiel, C. M. Ko, W. H. Ip, Y. Wang

Graduate Institute of Astronomy

Research output: Contribution to conference › Paper › peer-review

2 Scopus citations

Abstract

Fermi LAT has discovered two extended gamma-ray bubbles above and below the galactic plane. We propose that their origin is due to the permanent energy release in the Galactic center (GC) as a result of star accretion onto the central black hole. Shocks generated by these processes propagate into the Galactic halo and accelerate particles there. We show that electrons accelerated up to ∼ 10 TeV may be responsible for the observed gamma-ray emission of the bubbles as a result of inverse Compton (IC) scattering on the relic photons. We suggest that the Bubble could generate the flux of CR protons at energies > 10¹⁵ eV because the shocks in the Bubble have much larger length scales and longer lifetime in comparison with those in SNRs. This may explain the the CR spectrum above the knee.

Original language	English
Pages	10-13
Number of pages	4
DOIs	https://doi.org/10.7529/ICRC2011/V07/0589
State	Published - 2011
Event	32nd International Cosmic Ray Conference, ICRC 2011 - Beijing, China Duration: 11 Aug 2011 → 18 Aug 2011

Conference

Conference	32nd International Cosmic Ray Conference, ICRC 2011
Country/Territory	China
City	Beijing
Period	11/08/11 → 18/08/11

Keywords

Acceleration of particles
Galaxy: halo
Radiation mechanisms: non-thermal
Shock waves

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10.7529/ICRC2011/V07/0589

Cite this

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abstract = "Fermi LAT has discovered two extended gamma-ray bubbles above and below the galactic plane. We propose that their origin is due to the permanent energy release in the Galactic center (GC) as a result of star accretion onto the central black hole. Shocks generated by these processes propagate into the Galactic halo and accelerate particles there. We show that electrons accelerated up to ∼ 10 TeV may be responsible for the observed gamma-ray emission of the bubbles as a result of inverse Compton (IC) scattering on the relic photons. We suggest that the Bubble could generate the flux of CR protons at energies > 1015 eV because the shocks in the Bubble have much larger length scales and longer lifetime in comparison with those in SNRs. This may explain the the CR spectrum above the knee.",

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AU - Chernyshov, D. O.

AU - Cheng, K. S.

AU - Dogiel, V. A.

AU - Ko, C. M.

AU - Ip, W. H.

AU - Wang, Y.

PY - 2011

Y1 - 2011

N2 - Fermi LAT has discovered two extended gamma-ray bubbles above and below the galactic plane. We propose that their origin is due to the permanent energy release in the Galactic center (GC) as a result of star accretion onto the central black hole. Shocks generated by these processes propagate into the Galactic halo and accelerate particles there. We show that electrons accelerated up to ∼ 10 TeV may be responsible for the observed gamma-ray emission of the bubbles as a result of inverse Compton (IC) scattering on the relic photons. We suggest that the Bubble could generate the flux of CR protons at energies > 1015 eV because the shocks in the Bubble have much larger length scales and longer lifetime in comparison with those in SNRs. This may explain the the CR spectrum above the knee.

AB - Fermi LAT has discovered two extended gamma-ray bubbles above and below the galactic plane. We propose that their origin is due to the permanent energy release in the Galactic center (GC) as a result of star accretion onto the central black hole. Shocks generated by these processes propagate into the Galactic halo and accelerate particles there. We show that electrons accelerated up to ∼ 10 TeV may be responsible for the observed gamma-ray emission of the bubbles as a result of inverse Compton (IC) scattering on the relic photons. We suggest that the Bubble could generate the flux of CR protons at energies > 1015 eV because the shocks in the Bubble have much larger length scales and longer lifetime in comparison with those in SNRs. This may explain the the CR spectrum above the knee.

KW - Acceleration of particles

KW - Galaxy: halo

KW - Radiation mechanisms: non-thermal

KW - Shock waves

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T2 - 32nd International Cosmic Ray Conference, ICRC 2011

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Particle acceleration and the origin of gamma-ray emission from Fermi bubbles

Abstract

Conference

Keywords

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