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The Kepler mission has discovered thousands of exoplanets around variousstars with different spectral types (M, K, G, and F) and thus different massesand effective temperatures. Previous studies have shown that the planetoccurrence rate, in terms of average number of planets per star, drops withincreasing stellar effective temperature (Teff). In this paper, with the finalKepler Data Release (DR25) catalog, we revisit the relation between stellareffective temperature (as well as mass) and planet occurrence, but in terms ofthe fraction of stars with planets and the number of planets per planetarysystem (i.e. planet multiplicity). We find that both the fraction of stars withplanets and planet multiplicity decrease with increasing stellar temperatureand mass. Specifically, about 75% late-type stars (Teff<5000 K) haveKepler-like planets with an average planet multiplicity of ~2.8; while forearly-type stars (Teff>6500 K), this fraction and the average multiplicity falldown to ~35% and ~1.8, respectively. The decreasing trend in the fraction ofstars with planets is very significant with ${\Delta}$AIC> 30, though the trendin planet multiplicity is somewhat tentative with ${\Delta}$AIC~5. Our resultsalso allow us to derive the dispersion of planetary orbital inclinations inrelationship with stellar effective temperature. Interestingly, it is found tobe similar to the well-known trend between obliquity and stellar temperature,indicating that the two trends might have a common origin.

Occurrence and Architecture of Kepler Planetary Systems as Functions of Stellar Mass and Effective Temperature