Abstract
The classical nova GK Persei rivaled the brightness of Vega at the peak of its outburst in 1901. Early observations showed it to possess optical nebulosities apparently expanding at super-light velocities, later explained as "light echoes." Indeed, it was the first astronomical source in which such motion was observed. Subsequently, the expanding nova remnant has turned out to be the longest lived and most energetic among the classical novae and appears more like a supernova remnant (SNR) in miniature but evolving on human timescales. Here we report the results of multifrequency observations and archival research that confirm the presence of an ancient planetary nebula (PN), with an apparent hourglass morphology, ejected by the nova in a previous phase of evolution and into which the nova ejecta are now running. The 1901 nova outburst is therefore the first of ultimately very many that this system will undergo. Furthermore, from measurements of the proper motion of the central binary we can now understand the asymmetries observed both in the outer (ancient planetary) and inner (1901 nova ejecta) nebulae and their relationship to the longest lived of the light echoes first observed around 100 years ago. GK Persei may therefore be an important key to our understanding of interacting binary, PN, and SNR evolution.
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