Results 51 to 60 of about 123,043 (207)
Terrestrial planet formation in low eccentricity warm-Jupiter systems
, 2009 We examine the effect of giant planet migration on the formation of inner terrestrial planet systems. We consider situations in which the giant planet halts migration at semi-major axes in the range 0.13 - 1.7 AU due to gas disk dispersal. An N-body code
Fogg, M. J., Nelson, R. P.
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Infrared Non-detection of Fomalhaut b -- Implications for the Planet Interpretation [PDF]
, 2012 The nearby A4-type star Fomalhaut hosts a debris belt in the form of an eccentric ring, which is thought to be caused by dynamical influence from a giant planet companion.
Bent, John +5 more
core +1 more source
The Mass-Metallicity Relation for Giant Planets
, 2016 Exoplanet discoveries of recent years have provided a great deal of new data for studying the bulk compositions of giant planets. Here we identify 47 transiting giant planets ($20 M_\oplus < M < 20 M_{\mathrm{J}}$) whose stellar insolation is low enough (
Fortney, Jonathan J. +3 more
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The interplay between X-ray photoevaporation and planet formation [PDF]
, 2013 We assess the potential of planet formation instigating the early formation of a photoevaporation driven gap, up to radii larger than typical for photoevaporation alone.
Armitage, Philip J. +3 more
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Age Analysis of Extrasolar Planets: Insight from Stellar Isochrone Models
The Astronomical JournalThere is growing evidence from stellar kinematics and galactic chemical evolution suggesting that giant planets ( M _P ≥ 0.3 M _J ) are relatively young compared to the most commonly occurring population of small planets ( M _P < 0.3 M _J ).
C. Swastik +4 more
doaj +1 more source
The migration of gas giant planets in gravitationally unstable disks [PDF]
, 2015 Planets form in the disks of gas and dust that surround young stars. It is not known whether or not gas giant planets on wide orbits form the same way as Jupiter or form by the fragmentation of gravitationally unstable disks.
Stamatellos, Dimitris
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The Astronomical JournalWe report the discovery and confirmation of TOI-4465 b, a 1.25 R _J ${}_{-0.07{R}_{{\rm{J}}}}^{+0.08{R}_{{\rm{J}}}}$ , 5.89 M _J ± 0.26 M _J giant planet orbiting a G dwarf star at d ≃ 122 pc.
Zahra Essack +83 more
doaj +1 more source
EPJ Web of Conferences, 2013 The recognition that planets may survive the late stages of stellar evolution, and the prospects for finding them around White Dwarfs, are growing. We discuss two aspects governing planetary survival through stellar evolution to the White Dwarf stage ...
Bonsor Amy +4 more
doaj +1 more source
On the Formation of Gas Giant Planets on Wide Orbits
, 2006 A new suite of three dimensional radiative, gravitational hydrodynamical models is used to show that gas giant planets are unlikely to form by the disk instability mechanism at distances of ~100 AU to ~200 AU from young stars.
Boss, Alan P.
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A collisionless scenario for Uranus tilting
, 2010 The origin of the high inclination of Uranus' spin-axis (Uranus' obliquity) is one of the great unanswered questions about the Solar system. Giant planets are believed to form with nearly zero obliquity, and it has been shown that the present behaviour ...
Boué, Laskar, Murray-Clay, Ward
core +3 more sources