Results 131 to 140 of about 768 (162)

Decoding the formation of barred olivine chondrules: Realization of numerical replication. [PDF]

Sci Adv
Miura H, Morita T, Nakamura T, Watanabe K, Tsuchiyama A, Kimura Y, Koyama C.   +6 more
europepmc   +1 more source

The initial solar system abundance of ⁶⁰Fe and early core formation of the first asteroids. [PDF]

Sci Adv
Fang L, Moynier F, Chaussidon M, Limare A, Makhatadze GV, Villeneuve J.   +5 more
europepmc   +1 more source

Abundant supernova dust and heterogeneous aqueous alteration revealed by stardust in two lithologies of asteroid Bennu. [PDF]

Nat Astron
Nguyen AN, Seifert LB, Shimizu K, Thomas-Keprta K, Le L, Keller LP, Clemett SJ, Rahman Z, Barnes JJ, Connolly HC, Lauretta DS.   +10 more
europepmc   +1 more source

Perspectives on Mars Sample Return: A critical resource for planetary science and exploration. [PDF]

Proc Natl Acad Sci U S A
McSween HY, Hamilton VE, Farley KA.
europepmc   +1 more source

A 4,565-My-old record of the solar nebula field. [PDF]

Proc Natl Acad Sci U S A
Maurel C, Gattacceca J.
europepmc   +1 more source

Laboratory Investigation of Simultaneous Ultraviolet Photoprocessing and Temperature-Programmed Desorption of Interstellar Ice Analogs. [PDF]

ACS Earth Space Chem
Sarver CC, Walker CE, Widicus Weaver SL.
europepmc   +1 more source

Experimental quantification of hydrogen content in the Earth's core. [PDF]

Nat Commun
Huang D, Murakami M, Gerstl S, Liebske C.   +3 more
europepmc   +1 more source

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Planetesimals

2017
Processes governing the evolution of planetesimals are critical to understanding how rocky planets are formed, how water is delivered to them, the origin of planetary atmospheres, how cores and magnetic dynamos develop, and ultimately, which planets have the potential to be habitable.
openaire   +2 more sources

Radial Migration of Planetesimals

Astrophysics and Space Science, 1994
Planetesimals orbiting a protostar in a circumstellar disk are affected by gravitational interaction among themselves and by gas drag force due to disk gas. Within the Kyoto model of planetesimal accretion, the migration rate is interpreted as the inverse of the planetary formation time scale. Here, we study time scales of gravitational interaction and
Neuhäuser, R., Feitzinger, J.
openaire   +2 more sources