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Star Formation in Molecular Clouds: Observation and Theory
Star-formation (SF) processes occurring on the scale of giant molecular clouds (10 to the 6th solar masses and 10 to the 20th cm) or smaller are discussed, reviewing the results of recent theoreticalExpand
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Photoevaporation of Circumstellar Disks Due to External Far-Ultraviolet Radiation in Stellar Aggregates
When stars form within small groups (with N* ? 100-500 members), their circumstellar disks are exposed to relatively little extreme-ultraviolet (EUV; h? > 13.6 eV) radiation but a great deal ofExpand
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Spectral evolution of young stellar objects
An evolutionary sequence, from protostars to pre-main sequence stars, for the classification of young stellar objects is derived by comparing the predictions of the theoretical protostar models ofExpand
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Early evolution of stellar groups and clusters: environmental effects on forming planetary systems
This paper studies the dynamical evolution of young groups/clusters, with N = 100-1000 members, from their embedded stage out to ages of ~10 Myr. We use N-body simulations to explore how theirExpand
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We present a systematic evaluation of the agreement between the observed radii of 90 well-characterized transiting extrasolar giant planets and their corresponding model radii. Our model radii areExpand
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Sling amplification and eccentric gravitational instabilities in gaseous disks
An analytical description is presented of the modal mechanisms relevant to a recently discovered type of eccentric gravitational instability in nearly Keplerian disks. A quantum condition is derivedExpand
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Exclusion of Cosmic Rays in Protoplanetary Disks: Stellar and Magnetic Effects
Cosmic rays (CRs) are thought to provide an important source of ionization in the outermost and densest regions of protoplanetary disks; however, it is unknown to what degree they are physicallyExpand
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The T Tauri spectroscopic binary GW Orionis
The classical T Tauri star GW Ori is found to be a spectroscopic binary whose orbital period is 242 days. Radial velocity data are presented which show that GW Ori is a velocity variable, theExpand
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Infrared Spectra of Rotating Protostars
Earlier calculations of the infrared emission expected from stars in the process of being made are corrected to include the most important observable effects of rotation and generalized. An improvedExpand
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