The Interstellar Medium, Expanding Nebulae and Triggered Star Formation: Theory and Simulations
This brief brings together the theoretical aspects of star formation and ionized regions with the most up-to-date simulations and observations. Beginning with the basic theory of star formation, the physics of expanding HII regions is reviewed in detail and a discussion on how a massive star can give birth to tens or hundreds of other stars follows. The theoretical description of star formation is shown in simplified and state-of-the-art numerical simulations, describing in a more clear way how feedback from massive stars can trigger star and planet formation. This is also combined with spectacular images of nebulae taken by talented amateur astronomers. The latter is very likely to stimulate the reader to observe the structure of nebulae from a different point of view, and better understand the associated star formation therein.
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approximation Astrochemistry Astrophysics Bisbas chemical Collect and Collapse cometary tail considered cooling corresponding cosmic rays Crab Nebula creating D-type expansion dark nebula density distribution discussed emission nebulae equation evolution expanding H Expanding Nebulae expanding shell forbidden line formed fractal cloud Galaxy gas temperature globules grid-based H II region hence hydrogen atom inside interaction Interstellar Medium ionization front ionized medium ionizing radiation ionizing source Kallias Ioannidis kinetic energy known mass massive star material metals methods Milky MNRAS molecule Nebulae and Triggered neutral clumps neutral medium nucleosynthesis number density numerical simulations objects observed occurs phase photons planetary nebulae radiation driven implosion Raga Raga-I rarefied Rayleigh-Taylor instability recombination region expands result Sect shock front shows Smoothed Particle Hydrodynamics Solar system sound speed spherically symmetric stellar structure supernova explosion supernova remnants thermal pressure Tielens triggered star formation UV radiation Vishniac instability Voronoi tessellation wavelengths