.png){kind=icon}
.png){kind=icon}
Return
Astroparticles from X-Ray Binary Coronae
.png){kind=icon}
OA
AI
DOI：10.3847/2041-8213/ad887b.png)
.png){kind=icon}
Original request for help.png){kind=icon}
Share.png){kind=icon}
Save
Abstract
En 中文
The recent observation of high-energy neutrinos from the Galactic plane implies an abundant population of hadronic cosmic-ray sources in the Milky Way. We explore the role of the coronae of accreting stellar-mass black holes as such astroparticle emitters. We show that the particle acceleration and interaction timescales in the coronal region are tied to the compactness of the X-ray source. Thus, neutrino emission processes may similarly happen in the cores of active galactic nuclei and black hole X-ray binaries (XRBs), despite their drastically different masses and physical sizes. We apply the model to the well-measured XRB Cygnus X-1 and find that the cascaded gamma rays accompanying the neutrino emission naturally explain the GeV emission that only presents during the source's hard state, while the state-averaged gamma-ray emission explains the LHAASO observation above 20 TeV. We show that XRB coronae could contribute significantly to the Galactic cosmic-ray and Galactic plane neutrino fluxes. Our model predicts variable high-energy neutrino emission from bright Galactic XRBs that may be observed by IceCube and future neutrino observatories.
Keywords:
HIGH-ENERGY NEUTRINOS
BROAD-BAND SPECTRUM
GAMMA-RAY
CYGNUS X-1
ACCRETION FLOWS
MAGNETIC RECONNECTION
LUMINOSITY FUNCTION
TEV NEUTRINOS
BLACK-HOLES
EMISSION
Journal
IF:
11.7
Papers:
1.2W
Citations:
5.9W
