I.Introduction The formation process of massive O and B stars is arguably the least understood of all stars. The major observational and theoretical emphasis has been concentrated on low mass star formation during the past decade for a varitey of reasons, among which are: it is a more tractable problem than massive star formation and it is well matched with advances in instrumentation and evolution of theoretical ideas. Molecular cloud cores that give rise to low massstars have been isolated and intensely studied, providing evidence for the existence and properties of accretion disks, accretion rates, momentum shedding via HH-type jets and molecular outflows, etc. A corresponding advance in our understanding of massive stars has not occurred, although some progress has been made. Due to space limitations, this review will not be a general review of the subject, but instead will reflect some of my own particular interests although I will try to bias the topics covered to those where significant progress has been made. I will of necessity omit some interesting recent results of several groups, but many of these are discussed in posters and other reviews at this meeting. For a broad general review of newly formed massive stars see Churchwell (1990; 1991; 1993). Here, I will concentrate mostly on new results that have not been extensively discussed previously. In particular, I will discuss: 1) a possible technique to detect the hot, wind-shocked inner cavity within UC HI/regions which, at the same time, may also solve a problem with the origin of the disk component of the Fe XXV 6.7 kev line; 2) the variations of density and temperature within a particular cometary UC HI/region and consider implications for heating and cooling processes within the nebula; 3) high velocity molecular outflows associated with newly formed (or forming) massive stars; and 4) recent high spatial resolution observations of hot, dense molecular cloudlets associated with UC HI/regions and their possible relationship to the next generation of star formation.