It is really the simplicity that makes the story work so well. The movie itself is very simple it chronicles the growth of a couple and the impact their pet Labrador has on their family throughout their life. As I am sure many posters will repeat this phrase, if you've ever been a dog owner, this movie really rings true. Anyway, I was happy that she and my girlfriend were excited to see this. I was more excited by the fact that it was something that everyone could go and see including my mom, who doesn't venture out to the theater very often. This year's Christmas movie was 'Marley & Me'. The simulated populations of brown dwarfs also reveal that the phase of deuterium burning produces a distinctive feature in CMDs that should be detectable in ~50-100 Myr old clusters.Every year I go to see a movie on Christmas Day. Taken at face value, the present Pleiades data suggest that the L/T transition occurs at lower T eff for lower gravity objects, such as those found in young Galactic clusters. However, the same model is applied to the Pleiades brown dwarf sequence with less success. We also find that the transition from cloudy L dwarfs to cloudless T dwarfs slows down the evolution and causes a pileup of substellar objects in the transition region, in contradiction with previous studies. Instead of a single second parameter we find that variations in metallicity and cloud parameters, unresolved binaries, and possibly a relatively young population all play a role in defining the spread of brown dwarfs along the cooling sequence. We focus on near-infrared color-magnitude diagrams (CMDs) and on the nature of the 'second parameter' that is responsible for the scatter of colors along the T eff sequence. By combining the evolution calculation and our atmosphere models, we generate colors and magnitudes of synthetic populations of ultracool dwarfs in the field and in Galactic clusters. We develop a simple model for the evolution across the L/T transition. The L- to T-type ultracool dwarf transition can be accommodated within the Ackerman and Marley cloud model by varying the cloud sedimentation parameter. We discuss the sources of those differences and argue for the importance of the surface boundary condition provided by atmosphere models including clouds. While the predicted adiabatic evolution of luminosity with time is very similar to results of previous work, the remaining disagreements reveal the magnitude of current uncertainty in brown dwarf evolution theory. We present new evolution sequences for very low mass stars, brown dwarfs, and giant planets and use them to explore a variety of influences on the evolution of these objects.

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