The physics and dynamics of planetary nebulae

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Planetary nebulae are a classic subject in astrophysics, encompassing various physical processes in highly ionized gaseous media. These include the formation of emission lines under specific conditions and continuous emissions ranging from far ultraviolet to infrared and radio frequencies. The generation of exotic radiation forms predicted by atomic physics, along with methods for analyzing observed spectra and detecting physical and kinematic parameters of the radiating medium, are foundational to the physical theory of gaseous nebulae. This knowledge is crucial for understanding the diverse processes in the Universe, including those in gaseous envelopes around stars of different classes, stellar chromospheres and coronae, unstable stars, circumstellar clouds, and shells formed in nova and supernova explosions. It also applies to diffuse nebulae, the interstellar medium, interacting binary systems, emission-line galaxies, and quasars. Over the last thirty years, significant advancements have been made in understanding the nature of planetary nebulae. Notably, the discovery of radio emissions from PNs, predicted theoretically, and the unexpected powerful infrared emissions in both the continuum and emission lines have marked a turning point in this field.