Results 121 to 130 of about 3,499 (221)
Eos, Transactions American Geophysical Union, 2014 Planetesimals represent turning points in planetary formation, when the materials required for building planets are first incorporated into bodies with radii from tens to hundreds of kilometers or larger, and are sometimes differentiated into metallic cores and silicate mantles. These early celestial bodies are the accretionary step between the dust of
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, 1991 Formation of planetesimals is discussed. The following subject areas are covered: (1) nebular structure; (2) aerodynamics of the solid bodies in the nebula; (3) problems with gravitational instability; (4) particle growth by coagulation; properties of ...
Weidenschilling, Stuart J.
core
Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall
The Astrophysical JournalThere is growing evidence that planet formation begins early, within the ≲1 Myr Class 0/I phase, when infall dominates disk dynamics. Our goal is to determine if Class 0/I disks reach the conditions needed to form planetesimals (∼100 km planet building ...
Daniel Carrera +7 more
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, 2011 We present results of an image‐based numerical model aimed at quantifying the microsegregation and flow of liquid metal in meteorites prior to the onset of silicate melting. The sample material is the H6 chondrite Kernouvé.
Petford, Nick; id_orcid +4 more
core +1 more source
The Astrophysical JournalMercury’s core mass fraction (CMF) is 0.7, more than double that of the other rocky planets in the solar system, which have CMFs of 0.3 or lower. The origin of Mercury’s large, iron-rich core remains unknown. Adding to this mystery, an elusive population
Haniyeh Tajer +5 more
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Argon in β Pictoris–Entrapment and Release of Volatile in Disks
The Astrophysical JournalChemical compositions of planets reveal much about their formation environments. Such information is well sought-after in studies of solar system bodies and extrasolar ones.
Yanqin Wu +3 more
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The dissolution of planetesimals in electrostatic fields
Monthly Notices of the Royal Astronomical SocietyABSTRACT Planetesimals or smaller bodies in protoplanetary discs are often considered to form as pebble piles in current planet formation models. They are supposed to be large but loose, weakly bound clusters of more robust dust aggregates. This makes them easy prey for destructive processes.
F C Onyeagusi +3 more
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The Planetary Science JournalEarly solar system (SS) planetesimals constitute the parent bodies of most meteorites investigated today. Nucleosynthetic isotope anomalies of bulk meteorites have revealed a dichotomy between noncarbonaceous (NC) and carbonaceous (CC) groups ...
Teng Ee Yap +2 more
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Probing the formation of planetesimals in the Galactic Centre using Sgr A* flares
, 2015 Flares in X-ray and near-infrared are observed above the quiescent emission of the supermassive black hole (SBH) in the Galactic Centre (GC) at a rate of approximately once per day. One proposed energy source for these flares is the tidal disruption of
Hamers, A.S., Portegies Zwart, S.F.
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Shaken, not stirred: Inefficient mixing of CM- and CI-like materials
Astronomy & AstrophysicsContext. A recent study suggests that CM chondrite-like planetesimals formed in the vicinity of Saturn, in a pressure bump outside the gap carved by proto-Jupiter. While a fraction of these objects was implanted into the asteroid belt as a consequence of
Anderson S. E., Vernazza P., Brož M.
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