Early Initiation of Inner Solar System Formation at Dead-Zone Inner Edge. (arXiv:2110.06739v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Ueda_T/0/1/0/all/0/1">Takahiro Ueda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ogihara_M/0/1/0/all/0/1">Masahiro Ogihara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kokubo_E/0/1/0/all/0/1">Eiichiro Kokubo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Okuzumi_S/0/1/0/all/0/1">Satoshi Okuzumi</a>
The inner solar system possesses a unique orbital structure in which there
are no planets inside the Mercury orbit and the mass is concentrated around the
Venus and Earth orbits. The origins of these features still remain unclear. We
propose a novel concept that the building blocks of the inner solar system
formed at the dead-zone inner edge in the early phase of the protosolar disk
evolution, where the disk is effectively heated by the disk accretion. First,
we compute the dust evolution in a gas disk with a dead zone and obtain the
spatial distribution of rocky planetesimals. The disk is allowed to evolve both
by a viscous diffusion and magnetically-driven winds. We find that the rocky
planetesimals are formed in concentrations around $sim$ 1 au with a total mass
comparable to the mass of the current inner solar system in the early phase of
the disk evolution within $lesssim0.1$ Myr. Based on the planetesimal
distribution and the gas disk structure, we subsequently perform
textit{N}-body simulations of protoplanets to investigate the dynamical
configuration of the planetary system. We find that the protoplanets can grow
into planets without significant orbital migration because of the rapid
clearing of the inner disk by the magnetically-driven disk winds. Our model can
explain the origins of the orbital structure of the inner solar system. Several
other features such as the rocky composition can also be explained by the early
formation of rocky planetesimals.
The inner solar system possesses a unique orbital structure in which there
are no planets inside the Mercury orbit and the mass is concentrated around the
Venus and Earth orbits. The origins of these features still remain unclear. We
propose a novel concept that the building blocks of the inner solar system
formed at the dead-zone inner edge in the early phase of the protosolar disk
evolution, where the disk is effectively heated by the disk accretion. First,
we compute the dust evolution in a gas disk with a dead zone and obtain the
spatial distribution of rocky planetesimals. The disk is allowed to evolve both
by a viscous diffusion and magnetically-driven winds. We find that the rocky
planetesimals are formed in concentrations around $sim$ 1 au with a total mass
comparable to the mass of the current inner solar system in the early phase of
the disk evolution within $lesssim0.1$ Myr. Based on the planetesimal
distribution and the gas disk structure, we subsequently perform
textit{N}-body simulations of protoplanets to investigate the dynamical
configuration of the planetary system. We find that the protoplanets can grow
into planets without significant orbital migration because of the rapid
clearing of the inner disk by the magnetically-driven disk winds. Our model can
explain the origins of the orbital structure of the inner solar system. Several
other features such as the rocky composition can also be explained by the early
formation of rocky planetesimals.
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