Mostrando 1 - 20 Resultados de 64 Para Buscar 'protoplaneta~', tiempo de consulta: 4.68s Limitar resultados
  1. 1
    por Apai, Dániel, Lauretta, Dante S
    Publicado 2010
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    Protoplanetary dust: astrophysical and cosmochemical perspectives
  2. 2
    “…Chondrules are spherical silicate grains which formed from protoplanetary disk material, and as such provide an important record of the conditions of the Solar System in pre-planetary times. …”
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    Chondrules: records of protoplanetary disk processes
  3. 3
    por Chuburkov, Yu T
    Publicado 1999
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    Planetary Evidences of Magnetic Element Separation in Protoplanet Nebula
  4. 4
    “…In this article, we have reinvestigated the initial distribution of thermodynamic variables inside the protoplanets formed via gravitational instability having mass range [Formula: see text] ([Formula: see text]) by an embedded RKACeM(4,4) method assuming that the polytropic gas law holds in the protoplanets. …”
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    Online Artículo Texto
    An effective method in investigating structures of polytropic protoplanets formed via gravitational instability
  5. 5
    por Booth, Richard A., Clarke, Cathie J.
    Publicado 2016
    “…We have conducted the first comprehensive numerical investigation of the relative velocity distribution of dust particles in self-gravitating protoplanetary discs with a view to assessing the viability of planetesimal formation via direct collapse in such environments. …”
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    Online Artículo Texto
    Collision velocity of dust grains in self-gravitating protoplanetary discs
  6. 6
    “…Meteoritic chondrules are submillimeter spherules representing the major constituent of nondifferentiated planetesimals formed in the solar protoplanetary disk. The link between the dynamics of the disk and the origin of chondrules remains enigmatic. …”
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    Online Artículo Texto
    Early scattering of the solar protoplanetary disk recorded in meteoritic chondrules
  7. 7
    “…We infer that this secular evolution reflects admixing of pristine outer Solar System material to the thermally-processed inner protoplanetary disk associated with the accretion of mass to the proto-Sun. …”
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    Online Artículo Texto
    Isotopic evolution of the protoplanetary disk and the building blocks of Earth and Moon
  8. 8
    por Libourel, Guy, Portail, Marc
    Publicado 2018
    “…Chondrules, millimeter-sized igneous spherules comprising the major component of most chondritic meteorites, formed during the first 4 million to 5 million years of the evolution of the solar protoplanetary disk and, therefore, can potentially offer important constraints on the conditions in the disk, provided that the processes that led to their formation can be understood. …”
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    Online Artículo Texto
    Chondrules as direct thermochemical sensors of solar protoplanetary disk gas
  9. 9
    “…Concerning the heat transfer in the protoplanets, the mode of convection is taken into account. …”
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    Solving protoplanetary structure equations using Adomian decomposition method
  10. 10
    “…The main motivation and novel notion of this present communication is to implement the recently suggested fourth order with four stages embedded RKARMS(4,4) algorithm to examine its efficiency in reinvesting the structures of extrasolar protoplanets formed via disk instability which being presented in Paul et al. [1] (G.C. …”
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    Online Artículo Texto
    On the implementation of novel RKARMS(4,4) algorithm to study the structures of initial extrasolar giant protoplanets
  11. 11
    “…Meteorites display an isotopic composition dichotomy between noncarbonaceous (NC) and carbonaceous (CC) groups, indicating that planetesimal formation in the solar protoplanetary disk occurred in two distinct reservoirs. …”
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    Online Artículo Texto
    Natural separation of two primordial planetary reservoirs in an expanding solar protoplanetary disk
  12. 12
    “…Understanding the spatial variability of initial (26)Al/(27)Al in the solar system, i.e., ((26)Al/(27)Al)(0), is of prime importance to meteorite chronology, planetary heat production, and protoplanetary disc mixing dynamics. The ((26)Al/(27)Al)(0) of calcium-aluminum–rich inclusions (CAIs) in primitive meteorites (~5 × 10(−5)) is frequently assumed to reflect the ((26)Al/(27)Al)(0) of the entire protoplanetary disc, and predicts its initial (26)Mg/(24)Mg to be ~35 parts per million (ppm) less radiogenic than modern Earth (i.e., Δ′(26)Mg(0) = −35 ppm). …”
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    Online Artículo Texto
    Primordial formation of major silicates in a protoplanetary disc with homogeneous (26)Al/(27)Al
  13. 13
    por Kennedy, Grant M.
    Publicado 2020
    “…Whether these scenarios produce detectable eccentric rings within protoplanetary discs is unclear, but they nevertheless predict that narrow eccentric planetesimal rings should exist before the gas in protoplanetary discs is dispersed. …”
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    Online Artículo Texto
    The unexpected narrowness of eccentric debris rings: a sign of eccentricity during the protoplanetary disc phase
  14. 14
    “…Dynamic models of the protoplanetary disk indicate there should be large-scale material transport in and out of the inner Solar System, but direct evidence for such transport is scarce. …”
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    Online Artículo Texto
    Chondrules reveal large-scale outward transport of inner Solar System materials in the protoplanetary disk
  15. 15
    “…This book is based on the lectures by Philip Armitage and Wilhelm Kley presented at 45th Saas-Fee Advanced Course „From Protoplanetary Disks to Planet Formation“ of the Swiss Society for Astrophysics and Astronomy. …”
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    From protoplanetary disks to planet formation: Saas-Fee Advanced Course 45 Swiss Society for Astrophysics and Astronomy
  16. 16
    “…Pebbles of millimeter sizes are abundant in protoplanetary discs around young stars. Chondrules inside primitive meteorites—formed by melting of dust aggregate pebbles or in impacts between planetesimals—have similar sizes. …”
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    Online Artículo Texto
    A pebble accretion model for the formation of the terrestrial planets in the Solar System
  17. 17
    “…Terrestrial and sub-Neptune planets are expected to form in the inner (less than 10 au) regions of protoplanetary disks(1). Water plays a key role in their formation(2–4), although it is yet unclear whether water molecules are formed in situ or transported from the outer disk(5,6). …”
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    Online Artículo Texto
    Water in the terrestrial planet-forming zone of the PDS 70 disk
  18. 18
    “…The most abundant components of primitive meteorites (chondrites) are millimeter-sized glassy spherical chondrules formed by transient melting events in the solar protoplanetary disk. Using Pb-Pb dates of 22 individual chondrules, we show that primary production of chondrules in the early solar system was restricted to the first million years after the formation of the Sun and that these existing chondrules were recycled for the remaining lifetime of the protoplanetary disk. …”
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    Online Artículo Texto
    Early formation of planetary building blocks inferred from Pb isotopic ages of chondrules
  19. 19
    “…Chondritic meteorites are composed of primitive components formed during the evolution of the Solar protoplanetary disk. The oldest of these components formed by condensation, yet little is known about their formation mechanism because of secondary heating processes that erased their primordial signature. …”
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    Online Artículo Texto
    Rapid condensation of the first Solar System solids
  20. 20
    “…Diogenites are a group of meteorites that are derived from the interior of the largest protoplanet Vesta. They provide a unique opportunity to understanding together the internal structure and dynamic evolution of this protoplanet. …”
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    Online Artículo Texto
    Evidence of metasomatism in the interior of Vesta
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