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In this paper I examine the basic properties of the post-perihelion tails of the three brightest Kreutz sungrazers of the 19th and 20th centuries -- the Great March Comet of 1843 (C/1843 D1), the Great September Comet of 1882 (C/1882 R1), and Ikeya-Seki (C/1965 S1). 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