  Tidal disruption events (TDE) have been considered as cosmic-ray and neutrino
sources for a decade. We suggest two classes of new scenarios for high-energy
multi-messenger emission from TDEs that do not have to harbor powerful jets.
First, we investigate high-energy neutrino and gamma-ray production in the core
region of a supermassive black hole. In particular, we show that about 1-100
TeV neutrinos and MeV gamma-rays can efficiently be produced in hot coronae
around an accretion disk. We also study the consequences of particle
acceleration in radiatively inefficient accretion flows (RIAFs). Second, we
consider possible cosmic-ray acceleration by sub-relativistic disk-driven winds
or interactions between tidal streams, and show that subsequent hadronuclear
and photohadronic interactions inside the TDE debris lead to GeV-PeV neutrinos
and sub-GeV cascade gamma-rays. We demonstrate that these models should be
accompanied by soft gamma-rays or hard X-rays as well as optical/UV emission,
which can be used for future observational tests. Although this work aims to
present models of non-jetted high-energy emission, we discuss the implications
of the TDE AT2019dsg that might coincide with the high-energy neutrino
IceCube-191001A, by considering the corona, RIAF, hidden sub-relativistic wind,
and hidden jet models. It is not yet possible to be conclusive about their
physical association and the expected number of neutrinos is typically much
less than unity. We find that the most optimistic cases of the corona and
hidden wind models could be consistent with the observation of IceCube-191001A,
whereas jet models are unlikely to explain the multi-messenger observations.
