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The I-Xe chronometer and its constraints on the accretion and evolution of planetesimals
extinct radioisotopes iodine-xenon chondrites early solar system chronology
2017/4/10
We report a –1.6 ± 2.6 Myr (1s error) I-Xe age of the ungrouped achondrite NWA 7325 relative to the Shallowater
standard. We re-evaluate the calibration of the relative I-Xe dating system against the...
Planetesimals to protoplanets–II. Effect of debris on terrestrial planet formation
methods N-body simulations–methods numerical–Solar system formation–planetary systems formation
2015/12/25
In this paper, we extend our numerical method for simulating terrestrial planet formation to include dynamical friction from the unresolved debris component. In the previous work, we implemented a rub...
N-Body simulations of growth from 1 km planetesimals at 0.4 AU
Origin, Solar system Planetesimals Planetary formation Earth
2015/12/25
We present N-body simulations of planetary accretion beginning with 1 km radius planetesimals in orbit about a 1 M star at 0.4 AU. The initial disk of planetesimals contains too many bodies for any c...
PLANETESIMALS IN THE PRESENCE OF GIANT PLANET MIGRATION
Accretion accretion disks methods:n-body simulations planetary systems planets and satellites general
2015/12/25
We present N-body simulations illustrating how giant planet migration can significantly affect the conditions for the formation of interior terrestrial planets. A giant planet migrating through aswarm...
PLANETESIMALS TO PROTOPLANETS. I. EFFECT OF FRAGMENTATION ON TERRESTRIAL PLANET FORMATION
n-body simulations planetary systems solar system
2015/12/25
We present results from a dozen direct N-body simulations of terrestrial planet formation with various initial conditions. In order to increase the realism of our simulations and investigate theeffect...
Gravitational instability and clustering in a disk of planetesimals
stars planetary systems protoplanetary disks – gravitation – planets satellites formation
2015/12/25
For a long time, gravitational instability in the disk of planetesimals has been suspected to be the main engine responsible for the beginning of dust growth, its advantage being that it provides forr...
The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals? III. Sedimentation driven coagulation inside the snow-line
Methods Numerical Planets satellites formation Protoplanetary disks
2011/10/20
We investigate dust growth due to settling in a 1D vertical column of a protoplanetary disk. It is known from the observed 10 micron feature in disk SEDs, that small micron-sized grains are present at...
Forming Planetesimals by Gravitational Instability: II. How Dust Settles to its Marginally Stable State
Earth and Planetary Astrophysics (astro-ph.EP)
2010/12/23
Dust at the midplane of a circumstellar disk can become gravitationally unstable and fragment into planetesimals if the local dust-to-gas density ratio mu is sufficiently high. We simulate how dust se...
Forming Planetesimals by Gravitational Instability: I. The Role of the Richardson Number in Triggering the Kelvin-Helmholtz Instability
Earth and Planetary Astrophysics (astro-ph.EP)
2010/12/23
Gravitational instability (GI) of a dust-rich layer at the midplane of a gaseous circumstellar disk is one proposed mechanism to form planetesimals, the building blocks of rocky planets and gas giant ...