A "protoplanetary nebula" or "preplanetary nebula" is an astronomical object which is at the short-lived episode during a star's rapid stellar evolution between the late asymptotic giant branch phase and the subsequent planetary nebula phase. A PPN emits strongly in infrared radiation, and is a kind of reflection nebula. It is the second-from-the-last high-luminosity evolution phase in the life cycle of intermediate-mass stars . The name "protoplanetary nebula" is an unfortunate choice due to the possibility of confusion with the same term being sometimes employed when discussing the unrelated concept of protoplanetary disks. The name "protoplanetary nebula" is a consequence of the older term "planetary nebula", which was chosen due to early astronomers looking through telescopes and finding a similarity in appearance of planetary nebula to the gas giants such as Neptune and Uranus. To avoid any possible confusion, suggests employing a new term "preplanetary nebula" which does not overlap with any other disciplines of astronomy. They are often referred to as post-AGB stars, although that category also includes stars that will never ionize their ejected matter.
During the late asymptotic giant branch phase, when mass loss reduces the hydrogen envelope's mass to around 10 −2 for a core mass of 0.60 , a star will begin to evolve towards the blue side of the Hertzsprung–Russell diagram. When the hydrogen envelope has been further reduced to around 10 −3 , the envelope will have been so disrupted that it is believed further significant mass loss is not possible. At this point, the effective temperature of the star, "T" * , will be around 5,000 K and it is defined to be the end of the LAGB and the beginning of the PPN.
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