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The Horizontal Branch (HB) morphology in the color -- magnitude diagram ofthe Galactic globular clusters depends on many factors, and it is now firmlyestablished that the so-called Second Parameter is not just the cluster age asclaimed for several years. As a part of a wider program devoted to the searchfor the physical processes driving the Horizontal Branch Morphology, were-address here the problem of the extension of blue HB tails by introducing anew quantitative observable, B2/B+R+V where B2={Number of HB stars with(B-V)_0<-0.02}. We demonstrate that the environmental conditions within acluster clearly affect its HB morphology, in the sense that, in general, thehigher the cluster central density the higher is the relative number of starspopulating the most blue region of its HB.Comment: 14 pages, AASTEX latex, plus 3 .eps figures automatically enclosed,  needs the latex-macros aj_pt4.sty and epsf.sty -- To appear on The  Astronomical Journal, february 1996 issu

Horizontal Branch Morphology in Galactic Globular Clusters:Dense Environment is "A" Second Parameter