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Kepler planet candidate KOI-2700b (KIC 8639908b) with an orbital period of21.84 hours exhibits a distinctly asymmetric transit profile, likely indicativeof the emission of dusty effluents, and reminiscent of KIC 1255b. The host starhas $T_{\rm eff}$ = 4435 K, M = 0.63 $M_\odot$, and R = 0.57 $R_\odot$,comparable to the parameters ascribed to KIC 12557548. The transit egress canbe followed for ~25% of the orbital period, and, if interpreted as extinctionfrom a dusty comet-like tail, indicates a long lifetime for the dust grains ofmore than a day. We present a semi-physical model for the dust tailattenuation, and fit for the physical parameters contained in that expression.The transit is not sufficiently deep to allow for a study of thetransit-to-transit variations, as is the case for KIC 1255b; however, it isclear that the transit depth is slowly monotonically decreasing by a factor of~2 over the duration of the Kepler mission. The existence of a second starhosting a planet with a dusty comet-like tail would help to show that suchobjects may be more common and less exotic than originally thought. Accordingto current models, only quite small planets with Mp < 0.03 $M_\oplus$ arelikely to release a detectable quantity of dust. Thus, any "normal-looking"transit that is inferred to arise from a rocky planet of radius greater than~1/2 $R_\oplus$ should not exhibit any hint of a dusty tail. Conversely, if onedetects an asymmetric transit, due to a dusty tail, then it will be verydifficult to detect the hard body of the planet within the transit because, bynecessity, the planet must be quite small (i.e., < 0.3 $R_\oplus$).

KOI-2700b - A Planet Candidate With Dusty Effluents on a 22-Hour Orbit