tokens: the effects of AGN feedback in the evolution of its host galaxy. The galaxy is an isolated elliptical galaxy, and we assume in this work that the specific angular momentum of the gas is low. Physical processes like star formation and SNe Ia and II are taken into account. The inner boundary of the simulation is chosen so that the Bondi radius is resolved, which is crucial for the precise determination of the mass accretion rate of the AGN. According to the theory of black hole accretion, black hole accretion has two intrinsically different modes: cold and hot. They have quite different radiation and wind outputs and thus naturally correspond to two different feedback modes. They have been carefully discriminated and taken into account in the present work. We consider the feedback effects by both the radiation and wind in each mode. The two feedback modes have quite diverse names in the literature, e.g., the quasar (or radiative) and radio (or kinetic or maintenance) mode. Our present work indicates that these names are not only diverse but sometimes also misleading. For example, in terms of regulating the accretion rate of the black hole and star formation in the galaxy, feedback by the wind is always much more important than that by radiation. So, we suggest simply following the names of the black hole accretion mode and calling them the “cold feedback mode” and “hot feedback mode.” The most important distinctive feature of the present work is that we adopt the most updated AGN physics. This is especially the case for the radiation and wind from hot accretion flows, for which much progress has been made in recent years but has not been taken into account in most AGN feedback works (see a recent review by Yuan Narayan 2014 ). It also includes more precise descriptions of the wind in the cold mode that are obtained from recent new observations. These most updated AGN physics are summarized in the present paper. For the feedback effects, we have investigated the light curve of the AGN, the black hole growth, star formation, the AGN duty cycle, and the surface brightness of the galaxy. We have compared these results with previous works that have a very similar model framework to our work but different AGN physics. Significantly different results have been found in almost every aspect mentioned above. This indicates the crucial importance of having correct AGN physics. The main results obtained in this paper are summarized below. 1. We have compared the energy and momentum fluxes of the wind and radiation in the two feedback modes (Figure 1 ). Roughly speaking, in both modes, the power of radiation is larger than that of the wind, while the momentum flux is the opposite. However, the magnitude of the energy or momentum fluxes is not the only factor to determine which component, radiation or wind, is more important in the feedback. This is because the cross section of photon–particle interaction is orders of magnitude smaller than that of
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