Protoplanetary disk chemistry
KI Öberg, S Facchini… - Annual Review of …, 2023 - annualreviews.org
Planets form in disks of gas and dust around young stars. The disk molecular reservoirs and
their chemical evolution affect all aspects of planet formation, from the coagulation of dust …
their chemical evolution affect all aspects of planet formation, from the coagulation of dust …
Forming planets via pebble accretion
A Johansen, M Lambrechts - Annual Review of Earth and …, 2017 - annualreviews.org
The detection and characterization of large populations of pebbles in protoplanetary disks
have motivated the study of pebble accretion as a driver of planetary growth. This review …
have motivated the study of pebble accretion as a driver of planetary growth. This review …
Contemporary formation of early Solar System planetesimals at two distinct radial locations
The formation of planetesimals is expected to occur via particle-gas instabilities that
concentrate dust into self-gravitating clumps,–. Triggering these instabilities requires the …
concentrate dust into self-gravitating clumps,–. Triggering these instabilities requires the …
Thresholds for particle clumping by the streaming instability
The streaming instability (SI) is a mechanism to aerodynamically concentrate solids in
protoplanetary disks and trigger the formation of planetesimals. The SI produces strong …
protoplanetary disks and trigger the formation of planetesimals. The SI produces strong …
Rapid growth of gas-giant cores by pebble accretion
M Lambrechts, A Johansen - Astronomy & Astrophysics, 2012 - aanda.org
The observed lifetimes of gaseous protoplanetary discs place strong constraints on gas and
ice giant formation in the core accretion scenario. The approximately 10-Earth-mass solid …
ice giant formation in the core accretion scenario. The approximately 10-Earth-mass solid …
The dispersal of planet-forming discs: theory confronts observations
B Ercolano, I Pascucci - Royal Society Open Science, 2017 - royalsocietypublishing.org
Discs of gas and dust around million-year-old stars are a by-product of the star formation
process and provide the raw material to form planets. Hence, their evolution and dispersal …
process and provide the raw material to form planets. Hence, their evolution and dispersal …
Separating gas-giant and ice-giant planets by halting pebble accretion
M Lambrechts, A Johansen, A Morbidelli - Astronomy & Astrophysics, 2014 - aanda.org
In the solar system giant planets come in two flavours: gas giants (Jupiter and Saturn) with
massive gas envelopes, and ice giants (Uranus and Neptune) with much thinner envelopes …
massive gas envelopes, and ice giants (Uranus and Neptune) with much thinner envelopes …
The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths
E Chiang, G Laughlin - Monthly Notices of the Royal …, 2013 - academic.oup.com
Close-in super-Earths, with radii R≈ 2–5 R⊕ and orbital periods P< 100 d, orbit more than
half, and perhaps nearly all, Sun-like stars in the Universe. We use this omnipresent …
half, and perhaps nearly all, Sun-like stars in the Universe. We use this omnipresent …
Dynamics of protoplanetary disks
PJ Armitage - Annual Review of Astronomy and Astrophysics, 2011 - annualreviews.org
Protoplanetary disks are quasi-steady structures whose evolution and dispersal determine
the environment for planet formation. I review the theory of protoplanetary disk evolution and …
the environment for planet formation. I review the theory of protoplanetary disk evolution and …
Protoplanetary disks and their evolution
JP Williams, LA Cieza - Annual Review of Astronomy and …, 2011 - annualreviews.org
Flattened, rotating disks of cool dust and gas extending for tens to hundreds of astronomical
units are found around almost all low-mass stars shortly after their birth. These disks …
units are found around almost all low-mass stars shortly after their birth. These disks …