Does Jupiter form early? (based on Liu et al. Sci. Adv., in press)

by Dr Beibei Liu (Zhe Jiang University)

Tuesday 26 Apr 2022, 10:00 → 11:00 Asia/Shanghai

ONLINE

Abstract

Meteorites display an isotopic composition dichotomy between non-carbonaceous (NC) and carbonaceous (CC) groups, indicating that planetesimal formation in the solar protoplanetary disk occurred in two distinct reservoirs. The prevailing view is that a rapidly formed Jupiter acted as a barrier between these reservoirs. We show a fundamental inconsistency in this model: if Jupiter is an efficient blocker of drifting pebbles, then the interior NC reservoir is depleted by radial drift within a few hundred thousand years. If Jupiter lets material pass it, then the two reservoirs will be mixed. Instead, we demonstrate that the arrival of the CC pebbles in the inner disk is delayed for several million years by the viscous expansion of the protoplanetary disk. Our results support that Jupiter formed in the outer disk (>10 AU) and allowed a considerable amount of CC material to pass it and become accreted by the terrestrial planets.

Biography

Ph.D.: Peking University,2010-2015

Postdoc: University of Amsterdam,2015-2018; 2018-2020 Lund University;

Assistant Professor: 2020-now Zhejiang University

Chair

Fabo Feng

Division

Astronomy and Astrophysics

Other information

Video Record（for SJTU members）：

https://vshare.sjtu.edu.cn/play/e141f70bd898f1c4d51fbbe41e0cff88