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Recent observations of debris discs, believed to be made up of remnantplanetesimals, brought a number of surprises. Debris disc presence does notcorrelate with the host star's metallicity, and may anti-correlate with thepresence of gas giant planets. These observations contradict both assumptionsand predictions of the highly successful Core Accretion model of planetformation. Here we explore predictions of the alternative Tidal Downsizing (TD)scenario of planet formation. In TD, small planets and planetesimal debris ismade only when gas fragments, predecessors of giant planets, are tidallydisrupted. We show that these disruptions are rare in discs around highmetallicity stars but release more debris per disruption than their low [M/H]analogs. This predicts no simple relation between debris disc presence and hoststar's [M/H], as observed. A detected gas giant planet implies in TD that itspredecessor fragment was not disputed, potentially explaining why DDs are lesslikely to be found around stars with gas giants. Less massive planets shouldcorrelate with DD presence, and sub-Saturn planets ($M_{p} \sim 50\M_{\oplus}$) should correlate with DD presence stronger than sub-Neptunes($M_{p} \leq 15 \M_{\oplus}$). These predicted planet-DD correlations will bediluted and weakened in observations by planetary systems' long term evolutionand multi-fragment effects neglected here. Finally, although presentlydifficult to observe, DDs around M dwarf stars should be more prevalent thanaround Solar type stars.

Planets, debris and their host metallicity correlations