Results 91 to 100 of about 19,742 (238)

Radial transport and nebular thermal processing of millimeter‐sized solids in the Solar protoplanetary disk inferred from Cr‐Ti‐O isotope systematics of chondrules

Meteoritics &Planetary Science, Volume 59, Issue 12, Page 3282-3304, December 2024.
Abstract Understanding the material transport and mixing processes in the Solar protoplanetary disk provides important constraints on the origin of chemical and isotopic diversities of our planets. The limited extent of radial transport and mixing between the inner and outer Solar System has been suggested based on a fundamental isotopic dichotomy ...
Kohei Fukuda, Yuki Hibiya, Craig R. Kastelle, Katsuhiko Suzuki, Tsuyoshi Iizuka, Katsuyuki Yamashita, Thomas E. Helser, Noriko T. Kita   +7 more
wiley   +1 more source

Carbon In Protoplanetary Disks

, 2018
The carbon and oxygen content of the solids in protoplanetary disks plays an important role in defining the composition of giant planet atmospheres. I will discuss what we know about the distribution of carbonaceous material in the solar system and discuss potential processes influencing its radial distribution. I will also present modeling results for
openaire   +4 more sources

Resonant Relaxation in Protoplanetary Disks [PDF]

The Astronomical Journal, 1998
19 pages, 1 figure, LaTeX, submitted to ...
openaire   +3 more sources

The Determination of Protoplanetary Disk Masses [PDF]

, 2017
In this article we review the methods used to determine the gas and dust masses of protoplanetary disks, with an emphasis on the lesser characterized total gas mass. Our review encompasses all the indirect tracers and the methodology that is be used to isolate the hidden H2 via dust, CO, and HD emission.
Jonathan P. Williams, Edwin A. Bergin
openaire   +3 more sources

exoALMA. I. Science Goals, Project Design, and Data Products

The Astrophysical Journal Letters
Planet formation is a hugely dynamic process requiring the transport, concentration, and assimilation of gas and dust to form the first planetesimals and cores.
Richard Teague, Myriam Benisty, Stefano Facchini, Misato Fukagawa, Christophe Pinte, Sean M. Andrews, Jaehan Bae, Marcelo Barraza-Alfaro, Gianni Cataldi, Nicolás Cuello, Pietro Curone, Ian Czekala, Daniele Fasano, Mario Flock, Maria Galloway-Sprietsma, Himanshi Garg, Cassandra Hall, Iain Hammond, Thomas Hilder, Jane Huang, John D. Ilee, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Giuseppe Lodato, Cristiano Longarini, Ryan A. Loomis, Frédéric Masset, Francois Menard, Ryuta Orihara, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Leonardo Testi, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida, Brianna Zawadzki   +40 more
doaj   +1 more source

Toward an efficient second‐order method for computing the surface gravitational potential on spherical‐polar meshes

Astronomische Nachrichten, Volume 345, Issue 8, October 2024.
Abstract Astrophysical accretion discs that carry a significant mass compared with their central object are subject to the effect of self‐gravity. In the context of circumstellar discs, this can, for instance, cause fragmentation of the disc gas, and—under suitable conditions—lead to the direct formation of gas‐giant planets.
Oliver Gressel, Udo Ziegler
wiley   +1 more source

Conditions for Gravitational Instability in Protoplanetary Disks

, 2012
Gravitational instability is one of considerable mechanisms to explain the formation of giant planets. We study the gravitational stability for the protoplanetary disks around a protostar.
Kimura, Shigeo S., Tsuribe, Toru
core   +1 more source

Debris Disks: Probing Planet Formation

, 2018
Debris disks are the dust disks found around ~20% of nearby main sequence stars in far-IR surveys. They can be considered as descendants of protoplanetary disks or components of planetary systems, providing valuable information on circumstellar disk ...
A Bonsor, A Bonsor, A Bonsor, A Brandeker, A Gáspár, A Gáspár, A Hardy, A Moro-Martín, A Moór, A Schneider, A Shannon, A Shannon, AJ Mustill, AJ Mustill, AJW Richert, AM Hughes, AM Hughes, AM Lagrange, AP Jackson, AP Jackson, AV Krivov, AV Krivov, AV Krivov, B Ercolano, B Mennesson, B Sibthorpe, BP Bowler, C Eistrup, C Schüppler, C Vitense, CC Stark, Christine H. Chen, CM Lisse, CM Telesco, D Carrera, D Li, D Tamayo, DA Fischer, DA Golimowski, E Chiang, EJ Lee, ER Nesvold, ER Nesvold, F Geiler, F. Kiefer, G Bryden, GM Kennedy, GM Kennedy, GM Kennedy, H Beust, H Beust, H Genda, HF Levison, HYA Meng, HYA Meng, HYA Meng, J Lieman-Sifry, J Péricaud, J Wisdom, J. Olofsson, JC Augereau, JH Rhee, JM Carpenter, JN Winn, JS Greaves, JS Greaves, K Heng, KYL Su, L Matrà, L Matrà, L Matrà, L Ricci, LA Cieza, LE Strubbe, M Booth, M Booth, M Pan, MA MacGregor, MA MacGregor, MA Muñoz-Gutiérrez, Maryam Tabeshian, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, MC Wyatt, N Kains, N Pawellek, NA Kaib, ND Thureau, NM Phillips, O Panić, P Faber, P Kalas, P Thébault, Q Kral, Q Kral, Q. Kral, R Smith, S Marino, S Marino, S Marino, S Rappaport, S. Krijt, SJ Kenyon, SJ Kenyon, SJ Kenyon, SJ Kenyon, SN Raymond, T Currie, T Löhne, T Löhne, T Takeuchi, TD Pearce, TD Pearce, TS Boyajian, V Faramaz, W Lyra, WRF Dent, X Zheng, Y Hasegawa, Á Kóspál, É Morey   +131 more
core   +1 more source

Observations of inhomogeneities in protoplanetary disks

EPJ Web of Conferences, 2013
In this review I will give a brief overview of the latest observational constraints on the structure and dynamics of protoplanetary disks, with a particular emphasis on the topic of the conference: vortices.
Dullemond Cornelis
doaj   +1 more source

Planetary Migration in Protoplanetary Disks [PDF]

, 2018
The known exoplanet population displays a great diversity of orbital architectures, and explaining the origin of this is a major challenge for planet formation theories. The gravitational interaction between young planets and their protoplanetary disks provides one way in which planetary orbits can be shaped during the formation epoch.
openaire   +5 more sources