Massive star formation is the branch of astrophysics that studies the processes by which massive stars are born from clouds of gas and dust in the interstellar medium. Massive stars are defined as those with a mass greater than 8 times that of the Sun, and they play a crucial role in shaping the properties of their host galaxies. The process of massive star formation is thought to be initiated by the gravitational collapse of a dense molecular cloud core, which can be triggered by various mechanisms such as shockwaves from nearby supernovae or the gravitational influence of a passing molecular cloud. As the cloud core collapses under its own gravity, it heats up and forms a protostar surrounded by a rotating disk of gas and dust. The protostar continues to accrete material from the disk and grows in mass until it reaches the point where nuclear fusion reactions in its core can sustain the star against further collapse. The study of massive star formation involves observations at various wavelengths, from radio and infrared to X-ray and gamma-ray, as well as theoretical modeling of the physical processes involved. Researchers in this field aim to understand the conditions and mechanisms that lead to the formation of massive stars, as well as the impact of these stars on their surrounding environments.