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Fossilized condensa...
Fossilized condensation lines in the Solar System protoplanetary disk
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- Morbidelli, A. (author)
- Côte d'Azur Observatory
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- Bitsch, B. (author)
- Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science
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- Crida, A. (author)
- Institut Universitaire de France,Côte d'Azur Observatory
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- Gounelle, M. (author)
- Institut Universitaire de France,Versailles Saint-Quentin-en-Yvelines University
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- Guillot, T. (author)
- Côte d'Azur Observatory
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- Jacobson, S. (author)
- Côte d'Azur Observatory,University of Bayreuth
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- Johansen, A. (author)
- Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science
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- Lambrechts, M. (author)
- Côte d'Azur Observatory
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- Lega, E. (author)
- Côte d'Azur Observatory
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(creator_code:org_t)
- Elsevier BV, 2016
- 2016
- English 9 s.
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In: Icarus. - : Elsevier BV. - 0019-1035. ; 267, s. 368-376
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http://dx.doi.org/10...
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https://doi.org/10.1...
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Abstract
Subject headings
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- The terrestrial planets and the asteroids dominant in the inner asteroid belt are water poor. However, in the protoplanetary disk the temperature should have decreased below water-condensation level well before the disk was photo-evaporated. Thus, the global water depletion of the inner Solar System is puzzling. We show that, even if the inner disk becomes cold, there cannot be direct condensation of water. This is because the snowline moves towards the Sun more slowly than the gas itself. Thus the gas in the vicinity of the snowline always comes from farther out, where it should have already condensed, and therefore it should be dry. The appearance of ice in a range of heliocentric distances swept by the snowline can only be due to the radial drift of icy particles from the outer disk. However, if a planet with a mass larger than 20 Earth mass is present, the radial drift of particles is interrupted, because such a planet gives the disk a super-Keplerian rotation just outside of its own orbit. From this result, we propose that the precursor of Jupiter achieved this threshold mass when the snowline was still around 3 AU. This effectively fossilized the snowline at that location. In fact, even if it cooled later, the disk inside of Jupiter's orbit remained ice-depleted because the flow of icy particles from the outer system was intercepted by the planet. This scenario predicts that planetary systems without giant planets should be much more rich in water in their inner regions than our system. We also show that the inner edge of the planetesimal disk at 0.7 AU, required in terrestrial planet formation models to explain the small mass of Mercury and the absence of planets inside of its orbit, could be due to the silicate condensation line, fossilized at the end of the phase of streaming instability that generated the planetesimal seeds. Thus, when the disk cooled, silicate particles started to drift inwards of 0.7. AU without being sublimated, but they could not be accreted by any pre-existing planetesimals.
Subject headings
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
Keyword
- Cosmochemistry
- Origin, Solar System
- Planetesimals
- Solar Nebula
Publication and Content Type
- art (subject category)
- ref (subject category)
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