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The solid content of circumstellar disks is inherited from the interstellarmedium: dust particles of at most a micrometer in size. Protoplanetary disksare the environment where these dust grains need to grow at least 13 orders ofmagnitude in size. Our understanding of this growth process is far fromcomplete, with different physics seemingly posing obstacles to this growth atvarious stages. Yet, the ubiquity of planets in our galaxy suggests that planetformation is a robust mechanism. This chapter focuses on the earliest stages ofplanet formation, the growth of small dust grains towards the gravitationallybound "planetesimals", the building blocks of planets. We will introduce someof the key physics involved in the growth processes and discuss how they areexpected to shape the global behavior of the solid content of disks. We willconsider possible pathways towards the formation of larger bodies and concludeby reviewing some of the recent observational advances in the field.

Dust Evolution and the Formation of Planetesimals