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tokens: since the LC acts as a pin-hole, as well as due to their rareness. Single scattering, which leads to angular momentum change of ∼ j lc , is associated with impact parameter ∼( m * j cir / M bh j lc ) r . This impact parameter has to be ≳ R * , and in terms of r, m * , and M bh , strong scattering is relevant if This condition is easily satisfied for TDEs of main-sequence stars, and even for TDEs of red giants or binary break-ups, which leads to HVSs’ production, 3 it is satisfied for apoapsis distances r ∼ r h , which dominates the rate of TDEs and hyper velocity stars’ production. 6 SUMMERY AND DISCUSSION In this work, we have discussed the statistical properties of the pre-TDE dynamics and its correlations with the properties of the TDEs. In general, empty LC ( j d / j lc ≪ 1) is associated with non-violent TDEs of disrupted stars, in which stars that have already experienced significant tidal interaction with the SMBH experience TDE with marginal periastron (β − 1 ∼ j d / j lc ≪ 1). Similarly, full LC is associated with violent TDEs [] of non-disrupted stars. As for minority populations, different behaviour occurs for empty LC and full LC while considering single value of j d / j lc . In empty LC, a significant fraction () of the TDEs are non-typical being violent and involve mostly non-disrupted stars. This population of TDEs relates to the logarithmic fraction of stars that have been scattered into the LC by single large scatterings rather than by a large number of small scatterings. In the case of full LC, the fraction of non-violent TDEs of disrupted stars drops to zero for j d / j lc ≳ 0.3. However, significant minority population does arise for full LC, while assuming realistic j d / j lc distribution that arises due to the apoapsis distribution of the stars in the galaxy (Section 4 ). In this case, stars in orbits of marginal LC dominate the rate of TDEs, and as a result even if the LC is extremely full at the radius of influence [ j d, h = j d ( r h ) ≫ j lc ], an asymptotic fraction of of the TDEs involve stars in empty LC. Therefore, for any value of j d, h , at least a significant fraction () of the events are non-typical. Finally, in Section 5 , we discuss the value of j d, h / j lc in realistic astrophysical systems and find it to be ≫1 for red giants and for main-sequence stars. The physical consequences of previous interactions with the SMBH were not in the focus of the current work, and therefore are only briefly presented in the current section. For red giants, the role of previous interactions was already presented by MacLeod et al. ( 2013 ). According to this model, due to their inflated structure, red giants tend to ‘graze’ the LC, loose small amount of mass in each passage, and get back to equilibrium as an object of lower mass. This picture gives rise to ‘spoon feeding’ TDE instead of the violent typical TDE. This picture agrees perfectly with our expectation that most of the TDEs of red giants are expected to be