Results 41 to 50 of about 3,157,542 (333)
Multiple Populations of Extrasolar Gas Giants [PDF]
The Astrophysical Journal, 2019 Abstract There are two planetary formation scenarios: core accretion and gravitational disk instability. Based on the fact that gaseous objects are preferentially observed around metal-rich host stars, most extrasolar gaseous objects discovered to date are thought to have been formed by core accretion.
Shohei Goda, Taro Matsuo
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The Astrophysical Journal, 2023 In warm (equilibrium temperature
Benjamin Fleury +5 more
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Giant Spin Relaxation of an Ultracold Cesium Gas [PDF]
Physical Review Letters, 1998 We have measured the rate of inelastic collisions in a cloud of doubly polarized ground-state cesium atoms ( F=mF=4) confined in a magnetic trap for temperatures T between 8 and 70μK. We find a two-body rate coefficient varying as T−0.63. At 8 μK it reaches 4×10−12cm3s−1 which is 3 orders of magnitude larger than predicted, ruling out a Bose-Einstein ...
Soding J +4 more
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Journal of Petroleum Exploration and Production Technology, 2018 1986 saw the publication of a prognostic map for discovering giant oil and gas fields in the Andes in South America based on the recent block structure of the Earth’s crust.
Shelia Guberman, Yury Pikovskiy
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The Astronomical Journal, 2023 We confirm the planetary nature of two gas giants discovered by TESS to transit M dwarfs with stellar companions at wide separations. TOI-3984 A ( J = 11.93) is an M4 dwarf hosting a short-period (4.353326 ± 0.000005 days) gas giant ( M _p = 0.14 ± 0.03 ...
Caleb I. Cañas +32 more
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Growing the gas-giant planets by the gradual accumulation of pebbles [PDF]
Nature, 2015 It is widely held that the first step in forming gas-giant planets, such as Jupiter and Saturn, was the production of solid ‘cores’ each with a mass roughly ten times that of the Earth.
H. Levison, K. Kretke, M. Duncan
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THE EVOLUTION OF GAS GIANT ENTROPY DURING FORMATION BY RUNAWAY ACCRETION [PDF]
, 2016 We calculate the evolution of gas giant planets during the runaway gas accretion phase of formation, to understand how the luminosity of young giant planets depends on the accretion conditions.
D. Berardo, A. Cumming, G. Marleau
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The comparative effect of FUV, EUV and X-ray disc photoevaporation on gas giant separations [PDF]
, 2018 Gas giants' early (less than or similar to 5 Myr) orbital evolution occurs in a disc losing mass in part to photoevaporation driven by high energy irradiance from the host star.
J. Jennings, B. Ercolano, G. Rosotti
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Cloud and Gas Ionisation in Atmosphere of Gas-Giant Planets [PDF]
Proceedings of the International Astronomical Union, 2012 AbstractThe steady increase of the sample of know extrasolar planets broadens our knowledge and at the same time, reveals our lack of understanding. Habitability is a wide expression, needing planet formation theory and microphysics of cloud formation at the same time.
Declan A. Diver +4 more
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Accretion of Gas Giants Constrained by the Tidal Barrier [PDF]
The Astrophysical Journal, 2020 Abstract After protoplanets have acquired sufficient mass to open partial gaps in their natal protostellar disks, residual gas continues to diffuse onto horseshoe streamlines under the effect of viscous dissipation, and to meander in and out of the planets’ Hill sphere. Within the Hill sphere, the horseshoe streamlines intercept gas flow
Ya-Ping Li +3 more
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