tokens: (e.g. Narayan et al. 2012 ; Yuan, Wu Bu 2012b ; Yuan et al. 2015 ). In the hydrodynamic (HD) simulation, there is no magnetic field, wind is found to be driven by the combination of gas pressure gradient and centrifugal forces. In the magneto-hydrodynamic (MHD) simulation, it is found that wind is driven by the combination of gas pressure gradient, magnetic pressure gradient and centrifugal forces (Yuan et al. 2015 , see also Moller Sadowski 2015 ). Recently, observations of both LLAGNs (e.g. Tombesi et al. 2010 , 2014 ; Crenshaw Kramemer 2012 ; Wang et al. 2013 ; Cheung et al. 2016 ) and the hard state of black hole X-ray binaries (Homan et al. 2016 ) show that winds are present in hot accretion flows. The reason for the existence of wind is also investigated by analytical works (e.g. Begelman 2012 ; Gu 2015 ; Mosallanezhad, Bu Yuan 2016 ). Bu et al. ( 2016a , b ) study whether wind can be produced beyond the Bondi radius. In these studies, the gravity of nuclear star cluster is taken into account. It is found that the radial profile of the gravity becomes flatter when stars gravity is taken into account. Also, it is found that wind cannot be produced in the presence of star gravity. Wind production can occur only within the Bondi radius of hot accretion flows. The simulations introduced above neglect radiative cooling. Non-radiative simulations of hot accretion flows can only be applied when the black hole accretes at very low rate, , where is the Eddington accretion rate (Sadowski et al. 2017 ). With the increase of mass accretion rate, radiative cooling effects will become important. Strong radiative cooling can decrease the gas pressure. As mentioned above, gas pressure gradient is an important force for driving wind. We can expect that when radiation becomes strong, wind should become weak. In this paper, we study how the wind strength changes with mass accretion rate. We are interested in wind due to the following two reasons. First, wind can take away mass, which can change the density profile of accretion flows. The change of density profile can affect the emitted spectrum of an accretion flow (e.g. Quataert Narayan 1999 ; Yuan, Quataert Narayan 2003 ). Secondly, it is now widely believed that AGN feedback plays an important role in the evolution of their host galaxies (e.g. Ciotti Ostriker 1997 , 2001 , 2007 ; Proga, Stone Kallman 2000 ; Proga 2007 ; Kurosawa Proga 2009 ; Novak, Ostriker Ciotti 2011 ; Gan et al. 2014 , 2017 ; King Pounds 2015 ; Ciotti et al. 2017 ). Wind can push away the gas outside an AGN. This can reduce the feeding rate of the central black hole. Also, the star formation rate may also be changed (e.g. Ciotti et al. 2017 ). In order to study wind feedback, we first need to study the strength of wind. The effects of radiative cooling on hot accretion flow have been taken into account recently (e.g. Wu et al. 2016 ; Ryan et al. 2017 ). In these papers, the effects of radiative cooling on wind strength have not
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