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Chapter 3: The Origins and Evolution of Planetary Systems.

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Τίτλος: Chapter 3: The Origins and Evolution of Planetary Systems.
Συγγραφείς: Schaible MJ; School of Chemistry and Biochemistry, Georgia Institute of Technology, Atlanta, Georgia, USA., Todd ZR; Department of Earth and Space Sciences, University of Washington, Seattle, Washington, USA., Cangi EM; Department of Astrophysical and Planetary Sciences, University of Colorado Boulder, Boulder, Colorado, USA., Harman CE; NASA Ames Research Center, Moffett Field, California, USA., Hughson KHG; School of Earth and Atmospheric Science, Georgia Institute of Technology, Atlanta, Georgia, USA., Stelmach K; Department of Chemistry, University of Virginia, Charlottesville, Virginia, USA.
Πηγή: Astrobiology [Astrobiology] 2024 Mar; Vol. 24 (S1), pp. S57-S75.
Τύπος έκδοσης: Journal Article; Research Support, U.S. Gov't, Non-P.H.S.
Γλώσσα: English
Στοιχεία περιοδικού: Publisher: Mary Ann Liebert, Inc Country of Publication: United States NLM ID: 101088083 Publication Model: Print Cited Medium: Internet ISSN: 1557-8070 (Electronic) Linking ISSN: 15578070 NLM ISO Abbreviation: Astrobiology Subsets: MEDLINE
Imprint Name(s): Original Publication: Larchmont, N.Y. : Mary Ann Liebert, Inc., c2001-
Ιατρικοί όροι (MeSH): Planets* , Solar System*, Atmosphere/chemistry ; Extraterrestrial Environment/chemistry ; Earth, Planet ; Minor Planets ; Evolution, Planetary
Περίληψη: The materials that form the diverse chemicals and structures on Earth-from mountains to oceans and biological organisms-all originated in a universe dominated by hydrogen and helium. Over billions of years, the composition and structure of the galaxies and stars evolved, and the elements of life, CHONPS, were formed through nucleosynthesis in stellar cores. Climactic events such as supernovae and stellar collisions produced heavier elements and spread them throughout the cosmos, often to be incorporated into new, more metal-rich stars. Stars typically form in molecular clouds containing small amounts of dust through the collapse of a high-density core. The surrounding nebular material is then pulled into a protoplanetary disk, from which planets, moons, asteroids, and comets eventually accrete. During the accretion of planetary systems, turbulent mixing can expose matter to a variety of different thermal and radiative environments. Chemical and physical changes in planetary system materials occur before and throughout the process of accretion, though many factors such as distance from the star, impact history, and level of heating experienced combine to ultimately determine the final geophysical characteristics. In Earth's planetary system, called the Solar System, after the orbits of the planets had settled into their current configuration, large impacts became rare, and the composition of and relative positions of objects became largely fixed. Further evolution of the respective chemical and physical environments of the planets-geosphere, hydrosphere, and atmosphere-then became dependent on their local geochemistry, their atmospheric interactions with solar radiation, and smaller asteroid impacts. On Earth, the presence of land, air, and water, along with an abundance of important geophysical and geochemical phenomena, led to a habitable planet where conditions were right for life to thrive.
Contributed Indexing: Keywords: Cosmochemistry; Interstellar molecules; Planetary geology; Planetary science; Solar System
Entry Date(s): Date Created: 20240318 Date Completed: 20240320 Latest Revision: 20250728
Update Code: 20260130
DOI: 10.1089/ast.2021.0127
PMID: 38498821
Βάση Δεδομένων: MEDLINE
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  Data: The materials that form the diverse chemicals and structures on Earth-from mountains to oceans and biological organisms-all originated in a universe dominated by hydrogen and helium. Over billions of years, the composition and structure of the galaxies and stars evolved, and the elements of life, CHONPS, were formed through nucleosynthesis in stellar cores. Climactic events such as supernovae and stellar collisions produced heavier elements and spread them throughout the cosmos, often to be incorporated into new, more metal-rich stars. Stars typically form in molecular clouds containing small amounts of dust through the collapse of a high-density core. The surrounding nebular material is then pulled into a protoplanetary disk, from which planets, moons, asteroids, and comets eventually accrete. During the accretion of planetary systems, turbulent mixing can expose matter to a variety of different thermal and radiative environments. Chemical and physical changes in planetary system materials occur before and throughout the process of accretion, though many factors such as distance from the star, impact history, and level of heating experienced combine to ultimately determine the final geophysical characteristics. In Earth's planetary system, called the Solar System, after the orbits of the planets had settled into their current configuration, large impacts became rare, and the composition of and relative positions of objects became largely fixed. Further evolution of the respective chemical and physical environments of the planets-geosphere, hydrosphere, and atmosphere-then became dependent on their local geochemistry, their atmospheric interactions with solar radiation, and smaller asteroid impacts. On Earth, the presence of land, air, and water, along with an abundance of important geophysical and geochemical phenomena, led to a habitable planet where conditions were right for life to thrive.
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  Data: <i>Date Created: </i>20240318 <i>Date Completed: </i>20240320 <i>Latest Revision: </i>20250728
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