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We made a supplemental study of the superoutbursts and superhumps in SU UMastars by using the recently released Kepler public data of V1504 Cyg and V344Lyr. One of the superoutbursts in V1504 Cyg was preceded by a precursor normaloutburst which was well separated from the main superoutburst. The superhumpfirst appeared during the descending branch of the precursor normal outburstand it continued into quiescence (the deep dip between the precursor and themain superoutburst), and it began to grow in amplitude with the growth of themain superoutburst after quiescence ended. A similar phenomenon was alsoobserved in V344 Lyr. This observation demonstrates very clearly that thesuperoutburst was triggered by the superhump (i.e., by the tidal instability),supporting the thermal-tidal instability model. Smak (2013, Acta Astron., 63,109, arXiv:1301.0187) criticized our previous paper (Osaki and Kato, 2013,PASJ, 65, 50, arXiv:1212.1516) and challenged our main conclusion that variousobservational lines of evidence of V1504 Cyg support the thermal-tidalinstability model for the superoutbursts of SU UMa stars. We present ourdetailed accounts to all of his criticisms by offering clear explanations. Weconclude that the thermal-tidal instability model is after all only the viablemodel for the superoutbursts and superhumps in SU UMa stars.

A Further Study of Superoutbursts and Superhumps in SU UMa Stars by the Kepler Light Curves of V1504 Cygni and V344 Lyrae