Abstract
Many intermediate mass stars show signatures of circumstellar material. The young pre-main sequence Herbig Ae/Be stars often show flat or rising spectral energy distributions (SEDs) in the far-infrared, attributed to thermal emission of heated circumstellar dust, the remnant of star formation. A significant fraction of the much older main-sequence B and A-type stars also shows excess emission at λ ≥ 25µm (the so-called Vega-phenomenon, Backman and Paresce 1993), interpreted in terms of circumstellar disks maintained by destruction of asteroids and comets. The evolution from the circumstellar disks/envelopes of Herbig Ae/Be stars to Vega-like disks is, however, not well documented by observations (for an attempt using submm observations see Zuckerman and Becklin 1993). The evolutionary history, however, provides information on the lifetime of accretion disks around intermediate mass stars, and helps to clarify the role of these disks in stellar evolution, as well as defines the timescale for planet formation.
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