Neutrinos from the Galactic Center in the Light of HESS

We re-evaluate the event rate expected in km-scale detectors for neutrinos from the direction of the Galactic Center (GC) in light of recent results obtained by the HESS instrument for ∼TeV γ-radiation from this direction. Though (in the most plausible scenario) the re-evaluated event rate is smaller than that previously calculated—and here re-calculated—on the basis of EGRET data, the HESS GC γ-ray detection, together with the strong indications for an overabundance of cosmic rays coming from the GC at EeV energies, strengthen the expectation for a detectable, TeV-PeV GC neutrino signal from proton-proton interactions in that region. If the HESS-EeV cosmic ray anisotropy connection is correct, this signal will be detectable within a year and half for km-scale neutrino detectors in the Northern Hemisphere at super-TeV energies and, significantly, should also be detectable in 1.6 years by the South Polar IceCube detector at energies & 10 eV. The GC neutrino signal should also produce a detectable signal from neutrino showering and resonant W− production by νe’s in the volume of a km-scale detector. Subject headings: acceleration of particles — cosmic-rays — elementary particles — neutrinos — galactic center — radiation mechanisms: nonthermal — supernova remnants