TY - JOUR
T1 - Jupiter's evolution with primordial composition gradients
AU - Vazan, Allona
AU - Helled, Ravit
AU - Guillot, Tristan
N1 - Publisher Copyright:
© ESO 2018.
PY - 2018/2/1
Y1 - 2018/2/1
N2 - Recent formation and structure models of Jupiter suggest that the planet can have composition gradients and not be fully convective (adiabatic). This possibility directly affects our understanding of Jupiter's bulk composition and origin. In this Letter we present Jupiter's evolution with a primordial structure consisting of a relatively steep heavy-element gradient of 40 M⊙. We show that for a primordial structure with composition gradients, most of the mixing occurs in the outer part of the gradient during the early evolution (several 107 yr), leading to an adiabatic outer envelope (60% of Jupiter's mass). We find that the composition gradient in the deep interior persists, suggesting that ∼40% of Jupiter's mass can be non-adiabatic with a higher temperature than the one derived from Jupiter's atmospheric properties. The region that can potentially develop layered convection in Jupiter today is estimated to be limited to ∼10% of the mass.
AB - Recent formation and structure models of Jupiter suggest that the planet can have composition gradients and not be fully convective (adiabatic). This possibility directly affects our understanding of Jupiter's bulk composition and origin. In this Letter we present Jupiter's evolution with a primordial structure consisting of a relatively steep heavy-element gradient of 40 M⊙. We show that for a primordial structure with composition gradients, most of the mixing occurs in the outer part of the gradient during the early evolution (several 107 yr), leading to an adiabatic outer envelope (60% of Jupiter's mass). We find that the composition gradient in the deep interior persists, suggesting that ∼40% of Jupiter's mass can be non-adiabatic with a higher temperature than the one derived from Jupiter's atmospheric properties. The region that can potentially develop layered convection in Jupiter today is estimated to be limited to ∼10% of the mass.
KW - Planets and satellites: composition
KW - Planets and satellites: formation
KW - Planets and satellites: gaseous planets
KW - Planets and satellites: individual: Jupiter
KW - Planets and satellites: interiors
UR - http://www.scopus.com/inward/record.url?scp=85042623216&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201732522
DO - 10.1051/0004-6361/201732522
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AN - SCOPUS:85042623216
SN - 0004-6361
VL - 610
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - L14
ER -