Toward a Deterministic Model of Planetary Formation. I. A Desert in the Mass and Semimajor Axis Distributions of Extrasolar Planets
In an attempt to develop a deterministic theory for planet formation, we examine the accretion of cores of giant planets from planetesimals, gas accretion onto the cores, and their orbital migration.…
USING FU ORIONIS OUTBURSTS TO CONSTRAIN SELF-REGULATED PROTOSTELLAR DISK MODELS
- K. R. Bell, D. Lin
- Physics
- 8 December 1993
One-dimensional, convective, vertical structure models and one dimensional time-dependent, radial diffusion models are combined to create a self-consistent picture in which FU Orionis outbursts occur…
Transiting Exoplanet Survey Satellite (TESS)
- G. Ricker, J. Winn, J. Villasenor
- Physics, GeologyAstronomical Telescopes and Instrumentation
- 1 May 2009
The Transiting Exoplanet Survey Satellite (TESS ) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission.…
Orbital migration of the planetary companion of 51 Pegasi to its present location
- D. Lin, P. Bodenheimer, D. Richardson
- Physics, GeologyNature
- 18 April 1996
THE recent discovery1 and confirmation2 of a possible planetary companion orbiting the solar-type star 51 Pegasi represent a breakthrough in the search for extrasolar planetary systems. Analysis of…
Toward a Deterministic Model of Planetary Formation. II. The Formation and Retention of Gas Giant Planets around Stars with a Range of Metallicities
The apparent dependence of detection frequency of extrasolar planets on the metallicity of their host stars is investigated with Monte Carlo simulations using a deterministic core-accretion planet…
The Occurrence and Mass Distribution of Close-in Super-Earths, Neptunes, and Jupiters
The occurrence rate of close-in planets (with orbital periods less than 50 days), based on precise Doppler measurements of 166 Sun-like stars, is reported, indicating that theoretical models of planet formation predict a deficit of planets in the domain from 5 to 30 Earth masses and with orbital periods under 50 days are in fact well populated.
On the tidal interaction between protoplanets and the protoplanetary disk. III. Orbital migration of protoplanets
- D. Lin, J. Papaloizou
- Geology, Physics
- 15 October 1986
The tidal interaction between a protoplanet and a gaseous protoplanetary disk is investigated, and the dynamical evolution of the disk and the orbital migration of the protoplanet in a…
Structure, stability and evolution of Saturn's rings
- F. Bridges, A. Hatzes, D. Lin
- Physics, GeologyNature
- 1 May 1984
Recent data obtained from the Voyager spacecrafts and ground-based measurements indicate: (1) the rings have a thickness of at most 150 m (ref. 1) and probably several times less2,3; (2) the rings…
Remote sensing of planetary properties and biosignatures on extrasolar terrestrial planets.
- D. D. Des Marais, M. Harwit, N. Woolf
- Geology, PhysicsAstrobiology
- 1 June 2002
It is found that both the mid-IR and the visible to near-IR wavelength ranges offer valuable information regarding biosignatures and planetary properties; therefore both merit serious scientific consideration for TPF and Darwin.
Tidal Dissipation in Rotating Giant Planets
- G. Ogilvie, D. Lin
- Physics, Geology
- 8 October 2003
Many extrasolar planets orbit sufficiently close to their host stars that significant tidal interactions can be expected, resulting in an evolution of the spin and orbital properties of the planets.…
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