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tokens: of both the non-MAD and MAD states. Our main conclusions are summarized as follows: 1. High-energy particles at the first (strongest) shock during the debris circularization phase are unlikely to be produced, because the mass fallback rate exceeding the Eddington rate makes both the Compton drag and the proton–proton collision cooling very efficient. Since the shocked region is far from the black hole, the magnetic field is relatively weak. The weak magnetic field is another reason whythe stochastic acceleration of the protons becomes inefficient. 2. High-energy particles during the super-Eddington accretion phase of the non-MAD state are unlikely to be produced because of very efficient proton–proton collision cooling and Compton drag, even though the stochastic acceleration of the protons is more efficient because of the much stronger magnetic field than that of the first shock case. 3. Neutrinos and gamma-ray photons are produced by pions not only in the super-Eddington MAD scenario but also in the RIAF scenarios of both the non-MAD and MAD cases. However, the gamma-ray photons cannot escape from the source because of the large optical depth in the super-Eddington MAD state and because of the very efficient pair production in the RIAF cases. 4. In the RIAF phase, the protons can be accelerated up to with the other given appropriate parameters. The neutrino energy emitted at the peak of the spectrum is then estimated as . The neutrino emission is proportional to t −10/3 , which is steeper than the standard TDE decay rate. This indicates that one can potentially identify whether an RIAF that existed around an SMBH has a TDE origin or not. 5. In the super-Eddington MAD state, the stronger magnetic field than in the non-MAD case makes it possible to accelerate the protons up to ultrarelativistic energies. The dominant process to prevent the protons from accelerating strongly depends on the black hole mass. If the black hole mass is larger than , synchrotron cooling is the most dominant process. In this case, the protons are accelerated up to an energy of with the other given appropriate parameters. The neutrino energy at the peak of the spectrum is then estimated as . Otherwise, the Compton drag is more efficient process. In this case, the resultant energy of the protons increases at most up to . 6. In the super-Eddington MAD state, if M bh ≳ 10 7.7 M ⊙ , the neutrino light curve is proportional to , which is steeper than the standard TDE decay rate. On the other hand, it follows the decay rate with energy more than if . In both cases, the neutrino luminosity is of the order of the Eddington limit or the super-Eddington limit. Such a high neutrino luminosity and characteristic light curve give us the ability to judge whether the TDE disk is in the MAD state or not. 7. In the radiatively inefficient MAD state, the stronger magnetic field than in the non-MAD case makes it possible to accelerate the protons up to . The neutrino energy estimated