Sternbildung, or star formation, is the process by which dense regions within molecular clouds collapse under their own gravity to form stars. These clouds, primarily composed of hydrogen gas and dust, provide the necessary materials for star creation. As the gas and dust clump together, they heat up and eventually form a protostar, which is the early stage of a star. As the protostar continues to gather mass, nuclear fusion begins in its core, marking the transition to a main-sequence star. This process can take millions of years and is influenced by various factors, including the cloud's temperature, density, and the presence of nearby stars that can trigger further collapse.