Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores
With the recent realization that there likely are stably stratified regions in the interiors of both Jupiter and Saturn, we construct new nonadiabatic, inhomogeneous evolutionary models with the same microphysics for each that result at the present time in respectable fits for all major bulk observa...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/adad62 |
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| author | Ankan Sur Roberto Tejada Arevalo Yubo Su Adam Burrows |
| author_facet | Ankan Sur Roberto Tejada Arevalo Yubo Su Adam Burrows |
| author_sort | Ankan Sur |
| collection | DOAJ |
| description | With the recent realization that there likely are stably stratified regions in the interiors of both Jupiter and Saturn, we construct new nonadiabatic, inhomogeneous evolutionary models with the same microphysics for each that result at the present time in respectable fits for all major bulk observables for both planets. These include the effective temperature, radius, atmospheric heavy-element and helium abundances (including helium rain), and the lower-order gravity moments J _2 and J _4 . The models preserve from birth most of an extended “fuzzy” heavy-element core. Our predicted atmospheric helium mass fraction for Saturn is ∼0.2, close to some measured estimates but in disagreement with some published predictions. To preserve a fuzzy core from birth, the interiors of both planets must start out at lower entropies than would be used for traditional “hot start” adiabatic models, though the initial exterior mantle entropies can range from hot to warm start values. We do not see a helium ocean in Saturn’s interior, and both models have inner envelopes with significant Brunt–Väisälä frequencies; this region for Saturn at the current epoch is more extended, and in it, the Brunt is larger. The total heavy-element mass fraction in Jupiter and in Saturn is determined to be ∼14% and ∼26%, respectively, though there is some play in these determinations. |
| format | Article |
| id | doaj-art-c5e90c20e03048a0882927d873eb651e |
| institution | Kabale University |
| issn | 2041-8205 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Letters |
| spelling | doaj-art-c5e90c20e03048a0882927d873eb651e2025-02-05T17:52:12ZengIOP PublishingThe Astrophysical Journal Letters2041-82052025-01-019801L510.3847/2041-8213/adad62Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy CoresAnkan Sur0https://orcid.org/0000-0001-6635-5080Roberto Tejada Arevalo1https://orcid.org/0000-0001-6708-3427Yubo Su2https://orcid.org/0000-0001-8283-3425Adam Burrows3https://orcid.org/0000-0002-3099-5024Department of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08544, USA ; ankan.sur@princeton.eduDepartment of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08544, USA ; ankan.sur@princeton.eduDepartment of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08544, USA ; ankan.sur@princeton.eduDepartment of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08544, USA ; ankan.sur@princeton.eduWith the recent realization that there likely are stably stratified regions in the interiors of both Jupiter and Saturn, we construct new nonadiabatic, inhomogeneous evolutionary models with the same microphysics for each that result at the present time in respectable fits for all major bulk observables for both planets. These include the effective temperature, radius, atmospheric heavy-element and helium abundances (including helium rain), and the lower-order gravity moments J _2 and J _4 . The models preserve from birth most of an extended “fuzzy” heavy-element core. Our predicted atmospheric helium mass fraction for Saturn is ∼0.2, close to some measured estimates but in disagreement with some published predictions. To preserve a fuzzy core from birth, the interiors of both planets must start out at lower entropies than would be used for traditional “hot start” adiabatic models, though the initial exterior mantle entropies can range from hot to warm start values. We do not see a helium ocean in Saturn’s interior, and both models have inner envelopes with significant Brunt–Väisälä frequencies; this region for Saturn at the current epoch is more extended, and in it, the Brunt is larger. The total heavy-element mass fraction in Jupiter and in Saturn is determined to be ∼14% and ∼26%, respectively, though there is some play in these determinations.https://doi.org/10.3847/2041-8213/adad62Planetary structurePlanetary sciencePlanetary atmospheresExoplanet evolution |
| spellingShingle | Ankan Sur Roberto Tejada Arevalo Yubo Su Adam Burrows Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores The Astrophysical Journal Letters Planetary structure Planetary science Planetary atmospheres Exoplanet evolution |
| title | Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores |
| title_full | Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores |
| title_fullStr | Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores |
| title_full_unstemmed | Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores |
| title_short | Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores |
| title_sort | simultaneous evolutionary fits for jupiter and saturn incorporating fuzzy cores |
| topic | Planetary structure Planetary science Planetary atmospheres Exoplanet evolution |
| url | https://doi.org/10.3847/2041-8213/adad62 |
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