Did Jupiter's core form in the innermost parts of the Sun's protoplanetary disc?
(2016) In Monthly Notices of the Royal Astronomical Society 458(3). p.2962-2972- Abstract
Jupiter's core is generally assumed to have formed beyond the snow line. Here we consider an alternative scenario that Jupiter's core may have accumulated in the innermost part of the protoplanetary disc. A growing body of research suggests that small particles ('pebbles') continually drift inward through the disc. If a fraction of drifting pebbles is trapped at the inner edge of the disc, several Earth-mass cores can quickly grow. Subsequently, the core may migrate outward beyond the snow line via planet-disc interactions. Of course, to reach the outer Solar system Jupiter's core must traverse the terrestrial planet-forming region. We use N-body simulations including synthetic forces from an underlying gaseous disc to study how the... (More)
Jupiter's core is generally assumed to have formed beyond the snow line. Here we consider an alternative scenario that Jupiter's core may have accumulated in the innermost part of the protoplanetary disc. A growing body of research suggests that small particles ('pebbles') continually drift inward through the disc. If a fraction of drifting pebbles is trapped at the inner edge of the disc, several Earth-mass cores can quickly grow. Subsequently, the core may migrate outward beyond the snow line via planet-disc interactions. Of course, to reach the outer Solar system Jupiter's core must traverse the terrestrial planet-forming region. We use N-body simulations including synthetic forces from an underlying gaseous disc to study how the outward migration of Jupiter's core sculpts the terrestrial zone. If the outward migration is fast (τmig ~ 104 yr), the core simply migrates past resident planetesimals and planetary embryos. However, if its migration is slower (τmig ~ 105 yr) the core clears out solids in the inner disc by shepherding objects in mean motion resonances. In many cases, the disc interior to 0.5-1 AU is cleared of embryos and most planetesimals. By generating a mass deficit close to the Sun, the outward migration of Jupiter's core may thus explain the absence of terrestrial planets closer than Mercury. Jupiter's migrating core often stimulates the growth of another large (~Earth-mass) core - that may provide a seed for Saturn's core - trapped in an exterior resonance. The migrating core also may transport a fraction of terrestrial planetesimals, such as the putative parent bodies of iron meteorites, to the asteroid belt.
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- author
- Raymond, Sean N. ; Izidoro, Andre ; Bitsch, Bertram LU and Jacobson, Seth A.
- organization
- publishing date
- 2016-05-21
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- Planet-disc interactions, Planetary systems, Planets and satellites: Formation, Planets and satellites: Gaseous planets, Planets and satellites: Terrestrial planets, Protoplanetary discs
- in
- Monthly Notices of the Royal Astronomical Society
- volume
- 458
- issue
- 3
- pages
- 11 pages
- publisher
- Oxford University Press
- external identifiers
-
- scopus:84964734721
- wos:000375799000051
- ISSN
- 0035-8711
- DOI
- 10.1093/mnras/stw431
- language
- English
- LU publication?
- yes
- id
- 8855d698-cbd2-4bef-bfbe-a656da65f8cc
- date added to LUP
- 2016-10-04 15:50:09
- date last changed
- 2025-04-04 13:55:24
@article{8855d698-cbd2-4bef-bfbe-a656da65f8cc,
abstract = {{<p>Jupiter's core is generally assumed to have formed beyond the snow line. Here we consider an alternative scenario that Jupiter's core may have accumulated in the innermost part of the protoplanetary disc. A growing body of research suggests that small particles ('pebbles') continually drift inward through the disc. If a fraction of drifting pebbles is trapped at the inner edge of the disc, several Earth-mass cores can quickly grow. Subsequently, the core may migrate outward beyond the snow line via planet-disc interactions. Of course, to reach the outer Solar system Jupiter's core must traverse the terrestrial planet-forming region. We use N-body simulations including synthetic forces from an underlying gaseous disc to study how the outward migration of Jupiter's core sculpts the terrestrial zone. If the outward migration is fast (τ<sub>mig</sub> ~ 10<sup>4</sup> yr), the core simply migrates past resident planetesimals and planetary embryos. However, if its migration is slower (τ<sub>mig</sub> ~ 10<sup>5</sup> yr) the core clears out solids in the inner disc by shepherding objects in mean motion resonances. In many cases, the disc interior to 0.5-1 AU is cleared of embryos and most planetesimals. By generating a mass deficit close to the Sun, the outward migration of Jupiter's core may thus explain the absence of terrestrial planets closer than Mercury. Jupiter's migrating core often stimulates the growth of another large (~Earth-mass) core - that may provide a seed for Saturn's core - trapped in an exterior resonance. The migrating core also may transport a fraction of terrestrial planetesimals, such as the putative parent bodies of iron meteorites, to the asteroid belt.</p>}},
author = {{Raymond, Sean N. and Izidoro, Andre and Bitsch, Bertram and Jacobson, Seth A.}},
issn = {{0035-8711}},
keywords = {{Planet-disc interactions; Planetary systems; Planets and satellites: Formation; Planets and satellites: Gaseous planets; Planets and satellites: Terrestrial planets; Protoplanetary discs}},
language = {{eng}},
month = {{05}},
number = {{3}},
pages = {{2962--2972}},
publisher = {{Oxford University Press}},
series = {{Monthly Notices of the Royal Astronomical Society}},
title = {{Did Jupiter's core form in the innermost parts of the Sun's protoplanetary disc?}},
url = {{http://dx.doi.org/10.1093/mnras/stw431}},
doi = {{10.1093/mnras/stw431}},
volume = {{458}},
year = {{2016}},
}