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Cited by 231Astrophysics and Cosmic PhenomenaAstrophysical Phenomena and ObservationsGalaxies: Formation, Evolution, Phenomena

THE FERMI BUBBLES. I. POSSIBLE EVIDENCE FOR RECENT AGN JET ACTIVITY IN THE GALAXY

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Guo, Fulai, Mathews, William G.·2012·The Astrophysical Journal
DOI 10.1088/0004-637x/756/2/181
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Abstract

The Fermi Gamma-ray Space Telescope reveals two large gamma-ray bubbles in the Galaxy, which extend about 50° (∼10 kpc) above and below the Galactic center (GC) and are symmetric about the Galactic plane. Using axisymmetric hydrodynamic simulations with a self-consistent treatment of the dynamical cosmic ray (CR)–gas interaction, we show that the bubbles can be created with a recent active galactic nucleus (AGN) jet activity about 1–3 Myr ago, which was active for a duration of ∼0.1–0.5 Myr. The bipolar jets were ejected into the Galactic halo along the rotation axis of the Galaxy. Near the GC, the jets must be moderately light with a typical density contrast 0.001 ≲ η ≲ 0.1 relative to the ambient hot gas. The jets are energetically dominated by kinetic energy, and overpressured with either CR or thermal pressure which induces lateral jet expansion, creating fat CR bubbles as observed. The sharp edges of the bubbles imply that CR diffusion across the bubble surface is strongly suppressed. The jet activity induces a strong shock, which heats and compresses the ambient gas in the Galactic halo, potentially explaining the ROSAT X-ray shell features surrounding the bubbles. The Fermi bubbles provide plausible evidence for a recent powerful AGN jet activity in our Galaxy, providing new insights into the origin of the halo CR population and the channel through which massive black holes in disk galaxies release feedback energy during their growth.

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Crossref · 10.1088/0004-637x/756/2/181

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  • Jet-driven bubbles have been simulated in the context of the Fermi bubbles where the jet is injected for a short period of about 0.1-0.5 Myr with jet power Ljet∼(1-3)×10^44 erg/s, i.e. 0.2-0.5 Eddington luminosity, and total energy ∼10^57 erg.

    “Jet-driven bubbles have been simulated in the context of the FBs where the jet is injected for a short period of time ( ∼ 0 . 1 -0 . 5 Myr) with jet power, L jet ∼ (1 -3) × 10 44 erg s -1 i.e., 0 . 2 -0 . 5 L edd and total energy ∼ 10 57 erg (Guo et al. 2012; Guo & Mathews 2012; Yang et al. 2012, 2013; Yang & Ruszkowski 2017; Yang et al. 2022).”

    From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Guo et al. 2012

  • Jet-driven bubbles have been simulated in the context of the Fermi bubbles where the jet is injected for a short period of about 0.1-0.5 Myr with jet power Ljet∼(1-3)×10^44 erg/s, i.e. 0.2-0.5 Eddington luminosity, and total energy ∼10^57 erg.

    “Jet-driven bubbles have been simulated in the context of the FBs where the jet is injected for a short period of time ( ∼ 0 . 1 -0 . 5 Myr) with jet power, L jet ∼ (1 -3) × 10 44 erg s -1 i.e., 0 . 2 -0 . 5 L edd and total energy ∼ 10 57 erg (Guo et al. 2012; Guo & Mathews 2012; Yang et al. 2012, 2013; Yang & Ruszkowski 2017; Yang et al. 2022).”

    From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Guo & Mathews 2012

  • Although the contact discontinuity is expected to suffer from shear-driven Kelvin-Helmholtz instability, the presence of cosmic-ray diffusion and fluid viscosity can suppress such instabilities and produce the sharp edge for the Fermi bubbles.

    “Although the contact discontinuity is expected to suffer from the shear-driven Kelvin-Helmholtz instability (KHI), it is found that the presence of CR diffusion and fluid viscosity can suppress such instabilities and produce the sharp edge for the FBs (Guo & Mathews 2012).”

    From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Guo & Mathews 2012

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Authors
Guo, F., & Mathews, W. G.
Affiliations
University of California, Santa Cruz (US)
Corresponding author
Guo, Fulai
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2012-08-27
Volume
756
Issue
2
Pages
181
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1088/0004-637x/756/2/181
OpenAlex
W1999631552
Cited by
231
References
7
Citations by year
2026: 6 · 2025: 11 · 2024: 13 · 2023: 25 · 2022: 12 · 2021: 16 · 2020: 16 · 2019: 10 · 2018: 14 · 2017: 22 · 2016: 10 · 2015: 18 · 2014: 21 · 2013: 19 · 2012: 15
FWCI
9.38
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • arXiv (Cornell University)
Topics
  • Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Astrophysics and Cosmic Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Keywords
Fermi bubbles, Galactic halo, hydrodynamic modeling, cosmic ray diffusion, shock heating, Galactic Center, AGN feedback, Milky Way

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