An Exploration of Double Diffusive Convection in Jupiter as a Result of Hydrogen-Helium Phase Separation
| Autor: | J. J. Fortney, K. L. Moore, Christopher Mankovich, N. Nettelmann |
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| Rok vydání: | 2014 |
| Předmět: |
Convection
interiors [planets and satellites] 010504 meteorology & atmospheric sciences chemistry.chemical_element FOS: Physical sciences Astronomy & Astrophysics 01 natural sciences Jupiter Atmosphere 0103 physical sciences Thermal individual: Jupiter [planets and satellites] 010303 astronomy & astrophysics Helium convection 0105 earth and related environmental sciences Double diffusive convection Physics Earth and Planetary Astrophysics (astro-ph.EP) Astronomy Astronomy and Astrophysics Computational physics Heat flux chemistry physical evolution [planets and satellites] 13. Climate action Space and Planetary Science astro-ph.EP Astrophysics::Earth and Planetary Astrophysics Jupiter mass Astronomical and Space Sciences Astrophysics - Earth and Planetary Astrophysics |
| Zdroj: | Nettelmann, N; Fortney, JJ; Moore, K; & Mankovich, C. (2015). An exploration of double diffusive convection in Jupiter as a result of hydrogen-helium phase separation. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 447(4), 3422-3441. doi: 10.1093/mnras/stu2634. UC Santa Cruz: Retrieved from: http://www.escholarship.org/uc/item/0w2424vm MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol 447, iss 4 Monthly Notices of the Royal Astronomical Society, vol 447, iss 4 |
| DOI: | 10.48550/arxiv.1412.4202 |
| Popis: | Jupiter's atmosphere has been observed to be depleted in helium (Yatm~0.24), suggesting active helium sedimentation in the interior. This is accounted for in standard Jupiter structure and evolution models through the assumption of an outer, He-depleted envelope that is separated from the He-enriched deep interior by a sharp boundary. Here we aim to develop a model for Jupiter's inhomogeneous thermal evolution that relies on a more self-consistent description of the internal profiles of He abundance, temperature, and heat flux. We make use of recent numerical simulations on H/He demixing, and on layered (LDD) and oscillatory (ODD) double diffusive convection, and assume an idealized planet model composed of a H/He envelope and a massive core. A general framework for the construction of interior models with He rain is described. Despite, or perhaps because of, our simplifications made we find that self-consistent models are rare. For instance, no model for ODD convection is found. We modify the H/He phase diagram of Lorenzen et al. to reproduce Jupiter's atmospheric helium abundance and examine evolution models as a function of the LDD layer height, from those that prolong Jupiter's cooling time to those that actually shorten it. Resulting models that meet the luminosity constraint have layer heights of about 0.1-1 km, corresponding to ~10,-20,000 layers in the rain zone between ~1 and 3-4.5 Mbars. Present limitations and directions for future work are discussed, such as the formation and sinking of He droplets. Comment: accepted to MNRAS, 21 pages, 17 figures |
| Databáze: | OpenAIRE |
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