n the rush to go global, corporations are asking their employees to be I effective across distances never before mastered, depending on new innovations in communication technology to tie everyone together. These leaner companies are simultaneously emphasizing flexible team structures as the organizational molecule most responsive to rapid developments in products and markets. Teams of professionals, armed with laptop computers, fax-modems, E-mail, voice mail, videoconferencing, interactive databases, and fi-equent-flyer memberships, are being sent out to conduct business in this global arena.However, managers responsible for leading such teams have found that distance remains a very real dimension in human relations, despite electronic media and jet travel. A decision made in one country elicits an unexpected reaction from team members in another country. Remote offices fight for influence with the head office. Telephone conferences find This chapter is based on an earlier version, "Managing Geographic, Temporal and Cultural Distances in Distributed Work Groups," presented at the

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As an exoplanet orbits its host star it reflects and emits light, forming a distinctive phase curve 1,2 . By observing this light, we can study the atmosphere and surface of distant planets. The planets in our Solar System show a wide range of atmospheric phenomena, with stable wind patterns, changing storms, and evolving anomalies. Brown dwarfs also exhibit atmospheric variability 3,4 . Such temporal variability in the atmosphere of a giant exoplanet has not to date been observed. HAT-P-7 b is an exoplanet with a known offset in the peak of its phase curve 5,6 . Here we present variations in the peak offset ranging between -0.086 +0.033 -0.033 to 0.143 +0.040 -0.037 in phase, implying that the peak brightness repeatedly shifts from one side of the planet's substellar point to the other. The variability occurs on a timescale of tens to hundreds of days. These shifts in brightness are indicative of variability in the planet's atmosphere, and result from a changing balance of thermal emission and reflected flux from the planet's dayside. We suggest that variation in wind speed in the planetary atmosphere, leading to variable cloud coverage on the dayside and a changing energy balance, is capable of explaining the observed variation. Time (BJD-2454833)Peak Offset (Phase) Author ContributionsDJA obtained and detrended the data, developed and fit the phase curve models, implemented the atmospheric model, produced the figures and wrote the manuscript. EdM developed the discussion, contributed to the tests performed to check the results, and tested the results with his own models. HPO contributed to the phase curve model, and produced visual interpretations of the results. JBa developed the discussion of the atmospheric processes behind the peak offset variations. JBl provided the initial development of the phase curve model. NFS contributed to development of the figures. All authors commented on the manuscript.