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Spectral energy distributions of T Tauri stars - Disk flaring and limits on accretion
The Adams et al. (1987) conclusion that much of the IR excess emission in the spectral energy distribution of T Tauri stars arises from reprocessing of stellar radiation by a dusty circumstellar diskExpand
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PLANET FORMATION AROUND STARS OF VARIOUS MASSES : THE SNOW LINE AND THE FREQUENCY OF GIANT PLANETS
We use a semianalytic circumstellar disk model that considers movement of the snow line through evolution of accretion and the central star to investigate how gas giant frequency changes with stellarExpand
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The FU Orionis Phenomenon
▪ Abstract We summarize the properties of FU Orionis variables, and show how accretion disk models simply explain many peculiarities of these objects. FU Ori systems demonstrate that disk accretionExpand
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Spatial distribution of pre-main sequence stars in Taurus.
We derive characteristic properties of the nonrandom spatial distribution of pre-main-sequence stars in the Taurus-Auriga molecular cloud by applying several different statistical techniques. We findExpand
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THE MASS PROFILE OF THE GALAXY TO 80 kpc
The Hypervelocity Star Survey presents the currently largest sample of radial velocity measurements of halo stars out to 80 kpc. We apply spherical Jeans modeling to these data in order to derive theExpand
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An IRAS Survey of the Taurus-Auriga Molecular Cloud
IRAS data are used to search for young premain-sequence stars not previously associated with molecular cloud cores in the Taurus-Auriga region. NIR photometry and optical spectroscopy suggest thatExpand
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Variations on Debris Disks: Icy Planet Formation at 30-150 AU for 1-3 M☉ Main-Sequence Stars
We describe calculations for the formation of icy planets and debris disks at 30-150 AU around 1-3 M☉ stars. Debris disk formation coincides with the formation of planetary systems. As protoplanetsExpand
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The embedded young stars in the Taurus-Auriga molecular cloud. I - Models for spectral energy distributions
We describe radiative transfer calculations of infalling, dusty envelopes surrounding pre-main-sequence stars and use these models to derive physical properties for a sample of 21 heavily reddenedExpand
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