Results 31 to 40 of about 10,677 (209)

How to build Tatooine: reducing secular excitation in Kepler circumbinary planet formation

, 2012
Circumbinary planetary systems recently discovered by Kepler represent an important testbed for planet formation theories. Planetesimal growth in disks around binaries has been expected to be inhibited interior to ~10 AU by secular excitation of high ...
Rafikov, Roman R.
core   +1 more source

Planetesimal collisions in binary systems [PDF]

, 2010
We study the collisional evolution of km-sized planetesimals in tight binary star systems to investigate whether accretion towards protoplanets can proceed despite the strong gravitational perturbations from the secondary star.
Desidera, Guedes, Heppenheimer, Kley, Marzari, Neuhäuser, Paardekooper, Quintana, S.-J. Paardekooper, Stewart, Thébault, Thébault, Thébault, Thébault, Wiegert, Wyatt, Xie, Xie, Z. M. Leinhardt   +18 more
core   +1 more source

N-Body Simulation of Planetesimal Formation through Gravitational Instability of a Dust Layer in Laminar Gas Disk

, 2010
We investigate the formation process of planetesimals from the dust layer by the gravitational instability in the gas disk using local $N$-body simulations. The gas is modeled as a background laminar flow.
Barge, Barranco, Chiang, Coradini, Daisaka, Eiichiro Kokubo, Gómez, Ishitsu, Johansen, Johansen, Johansen, Landau, Michikoshi, Michikoshi, Michikoshi, Richardson, Safronov, Sekiya, Sekiya, Shu-ichiro Inutsuka, Shugo Michikoshi, Wakita, Ward, Weidenschilling, Weidenschilling, Yamoto, Youdin, Youdin, Youdin, Youdin   +29 more
core   +1 more source

Deciphering the Origin of the Regular Satellites of Gaseous Giants - Iapetus: the Rosetta Ice-Moon [PDF]

, 2009
Here we show that Iapetus can serve to discriminate between satellite formation models. Its accretion history can be understood in terms of a two-component gaseous subnebula, with a relatively dense inner region, and an extended tail out to the location ...
Atreya, Ayliffe, Bai, Baker, Bate, Beckwith, Bell, Benz, Birnstiel, Bodenheimer, Bottke, Brauer, Bronshten, Brown, Buie, Buratti, Canup, Castillo-Rogez, Castillo-Rogez, Chabot, Charnoz, Charnoz, Charnoz, Chyba, Currie, Cuzzi, Cuzzi, Cuzzi, Davis, Dodson-Robinson, Dohnanyi, Dominik, Dominik, Dullemond, Durham, Ellsworth, Estrada, Ghosh, Hayashi, Hobbs, Housen, Hubickyj, Ignacio Mosqueira, Jewitt, Johansen, Johnson, Kenyon, Koponen, Kretke, Lin, Lunine, Lyra, McKinnon, Merk, Morbidelli, Morbidelli, Morfill, Moses, Mosqueira, Mosqueira, Mosqueira, Owen, Paul R. Estrada, Person, Podolak, Pollack, Pollack, Pollack, Prialnik, Prialnik, Prinn, Rafikov, Ryan, Scott, Sebastien Charnoz, Smoluchowski, Sohl, Stern, Stevenson, Svetsov, Tamayo, Tremaine, Turner, Ward, Weidenschilling, Weidenschilling, Wetherill, Wong, Youdin, Young, Zahnle, Zahnle   +91 more
core   +2 more sources

3D SR‐μXCT analysis for lithology detection: Application to Ryugu sample A0159

Meteoritics &Planetary Science, EarlyView.
Abstract Extraterrestrial breccia samples are formed through impact‐related processes that combine the fragments of distinct lithologies. As such, they are valuable indicators of the complex formation and evolution history of planetesimals in our solar system.
Léna Jossé, Zélia Dionnet, Alice Aléon‐Toppani, Rosario Brunetto, Andrew King, Emmanuel Gardés, Eva Heripré, Damien Loizeau, Sasha Cryan, Kentaro Hatakeda   +9 more
wiley   +1 more source

Metallicity of the Massive Protoplanets Around HR 8799 If Formed by Gravitational Instability

, 2009
The final composition of giant planets formed as a result of gravitational instability in the disk gas depends on their ability to capture solid material (planetesimals) during their 'pre-collapse' stage, when they are extended and cold, and contracting ...
Alexander, Bodenheimer, Boley, Boss, Boss, Cameron, Cuzzi, Decampli, Dodson-Robinson, Durisen, Greenzweig, Guillot, Haghighipour, Helled, Helled, Helled, Henyey, Hubickyj, Ida, Johansen, Kalas, Klahr, Mamatsashvili, Marley, Marois, Mayer, Mayer, Mayer, Morbidelli, P. Bodenheimer, Pollack, Pollack, R. Helled, Rafikov, Rice, Saumon   +35 more
core   +1 more source

Atmospheric Mass Loss During Planet Formation: The Importance of Planetesimal Impacts [PDF]

, 2014
We quantify the atmospheric mass loss during planet formation by examining the contributions to atmospheric loss from both giant impacts and planetesimal accretion. Giant impacts cause global motion of the ground.
Sari, Re'em, Schlichting, Hilke, Yalinewich, Almog   +2 more
core   +2 more sources

Experimental constraints on the origin of metal and carbon in ureilite meteorites

Meteoritics &Planetary Science, EarlyView.
Abstract Ureilites are carbon‐rich ultramafic achondrites that display unique textures, including strips of metal and carbon phases situated along grain boundaries and in fractures. Shock metamorphism observed in ureilites suggests an episode of brittle deformation caused by impact disruption of their parent body.
Nicolas P. Walte, Max Collinet, Cyrena A. Goodrich   +2 more
wiley   +1 more source

Oligarchic Growth of Protoplanets in Planetesimal Rings

The Astrophysical Journal
In the standard planet formation scenario, planetesimals are assumed to form throughout the protoplanetary disk and to be smoothly distributed in the radial direction except for the snowline.
Yuki Kambara, Eiichiro Kokubo
doaj   +1 more source

Chromite in main group pallasite meteorites: Accessory mineral tracing planetesimal differentiation

Meteoritics &Planetary Science, EarlyView.
Abstract Main group pallasite meteorites (PMG) are samples of an early, highly differentiated magmatic planetesimal dominated by olivine and metal‐sulfide‐phosphide assemblages with accessory chromite among other phases. This mineralogy reflects mantle‐ and core‐related reservoirs, but the relative contributions of each and the overall petrogenesis are
Seann J. McKibbin, Lutz Hecht, Matthew S. Huber, Christina Makarona, Stepan M. Chernonozhkin, Philippe Claeys, Steven Goderis   +6 more
wiley   +1 more source