Results 1 to 10 of about 7,582 (209)

Particle confinement in a non-axisymmetric protoplanetary nebula [PDF]

Open Astronomy, 1999
Fuente Marcos C. de la, Barge P.
doaj   +4 more sources

Igneous processes in the small bodies of the Solar System I. Asteroids and comets [PDF]

iScience, 2023
Summary: Igneous processes were quite widespread in the small bodies of the Solar System (SBSS) and were initially fueled by short-lived radioisotopes, the proto-Sun, impact heating, and differentiation heating.
Giovanni Leone, Hiroyuki K.M. Tanaka
doaj   +2 more sources

Igneous meteorites suggest Aluminium-26 heterogeneity in the early Solar Nebula [PDF]

Nature Communications, 2023
The short-lived radionuclide aluminium-26 (26Al) isotope is a major heat source for early planetary melting. The aluminium-26 – magnesium-26 (26Al-26Mg) decay system also serves as a high-resolution relative chronometer.
Evgenii Krestianinov, Yuri Amelin, Qing-Zhu Yin, Paige Cary, Magdalena H. Huyskens, Audrey Miller, Supratim Dey, Yuki Hibiya, Haolan Tang, Edward D. Young, Andreas Pack, Tommaso Di Rocco   +11 more
doaj   +2 more sources

Igneous processes in the small bodies of the Solar System II: Small satellites and dwarf planets [PDF]

iScience
Summary: Evidence of hot and cold igneous processes has been reported in small satellites and dwarf planets of the Solar System. Olivine and pyroxenes were detected in the spectral bands of both small satellites and dwarf planets.
Giovanni Leone, Hiroyuki Tanaka
doaj   +2 more sources

UV Monochromatic Imaging of the Protoplanetary Nebula Hen 3-1475 Using HST STIS [PDF]

Galaxies, 2018
Collimated outflows and jets play a critical role in shaping planetary nebulae (PNe), especially in the brief transition from a spherical AGB envelope to an aspherical PN, which is called the protoplanetary nebula (pPN) phase.
Xuan Fang, Martín A. Guerrero, Ana I. Gómez de Castro, Jesús A. Toalá, Bruce Balick, Angels Riera   +5 more
doaj   +2 more sources

Implications for Chondrule Formation Regions and Solar Nebula Magnetism from Statistical Reanalysis of Chondrule Paleomagnetism

The Planetary Science Journal, 2023
Converging lines of evidence show that protoplanetary disks are complex environments hosting spatial and temporal variability at multiple scales.
Roger R. Fu, Sarah C. Steele, Jacob B. Simon, Richard Teague, Joan Najita, David Rea   +5 more
doaj   +1 more source

Formation of the First Planetesimals via the Streaming Instability in Globally Turbulent Protoplanetary Disks?

The Astrophysical Journal, 2023
Using self-consistent models of turbulent particle growth in an evolving protoplanetary nebula of solar composition, we find that recently proposed local metallicity and Stokes number criteria necessary for the streaming instability to generate ...
Paul R. Estrada, Orkan M. Umurhan
doaj   +1 more source

The composition of the protosolar disk and the formation conditions for comets [PDF]

, 2015
Conditions in the protosolar nebula have left their mark in the composition of cometary volatiles, thought to be some of the most pristine material in the solar system.
A. Dutrey, A. Kouchi, A.E. Glassgold, A.G.G.M. Tielens, A.I. Vasyunin, A.L. Cochran, A.N. Heays, A.Z. Dolginov, B. Silvi, B.P. Bonev, B.P. Bonev, B.P. Bonev, C. Alexander, C. Ceccarelli, C. Ceccarelli, C. Ceccarelli, C. Dominik, C. Qi, C. Qi, C. Qi, C. Qi, C. Salyk, C. Tornow, C. Tornow, C. Tornow, C. Walsh, C. Walsh, C.E. Woodward, C.P. Dullemond, D. Bockelée-Morvan, D. Bockelée-Morvan, D. Bockelée-Morvan, D. Bockelée-Morvan, D. Bockelée-Morvan, D. Gautier, D. Harsono, D. Heinzeller, D. Hutsemékers, D. Kozlowski, D. Semenov, D. Semenov, D.C. Lis, E. Gibb, E. Herbst, E. Jehin, E. Lellouch, E. Roueff, E. S. Wirström, E. Zicler, E.D. Young, E.K. Jessberger, E.L. Gibb, E.S. Wirström, E.S. Wirström, F. Hersant, F. Pauzat, F.C. Adams, F.J. Ciesla, F.J. Ciesla, G. Buntkowsky, G. Bussolin, G. Cremonese, G. Kresse, G. Kresse, G. Notesco, G.J. Flynn, G.J. Villanueva, G.L. Villanueva, G.S. Mathews, H. Kawakita, H. Kawakita, H. Kawakita, H. Kawakita, H. Yurimoto, H. Yurimoto, I. Gregorio-Monsalvo de, I. Pater de, I. Pater de, J. Crovisier, J. Crovisier, J. Crovisier, J. Crovisier, J. Crovisier, J. Schönke, J.-E. Lee, J.C. Mottram, J.E. Heidenreich III, J.F. Hawley, J.F. Hawley, J.I. Lunine, J.J. Kavelaars, J.K.J. Fogel, J.P. Perdew, J.R. Lyons, J.R. Najita, J.S. Carr, J.S. Lewis, J.S. Mathis, K. Altwegg, K. France, K. Hashimoto, K. Nagashima, K. Saigo, K. Willacy, K. Willacy, K. Willacy, K. Willacy, K. Willacy, K. Willacy, K.D. McKeegan, K.I. Öberg, K.M. Chick, K.M. Pontoppidan, K.M. Pontoppidan, K.M. Pontoppidan, K.M. Pontoppidan, K.Y. Furuya, L. Pagani, L. Paganini, L. Podio, L.I. Cleeves, L.I. Cleeves, L.I. Cleeves, L.R. Nittler, M. Ali-Dib, M. Ali-Dib, M. Asplund, M. Calatayud, M. Doronin, M. Hassig, M. Ilgner, M. Ilgner, M. Ilgner, M. Pettini, M.A. DiSanti, M.F. A’Hearn, M.J. Mumma, M.J. Mumma, M.J. Mumma, M.R. Hogerheijde, M.V. Persson, N. Biver, N. Dello Russo, N. Dello Russo, N. Dello Russo, N. Fray, N. Iro, N. Watanabe, N.J. Turner, N.J. Turner, N.J. Turner, O. Mousis, O. Mousis, O. Mousis, O. Mousis, O. Mousis, O. Mousis, O. Mousis, O. Mousis, O. Mousis, O. Mousis, O. Mousis, P. Caselli, P. D’Alessio, P. Eberhardt, P. Eberhardt, P. Gast, P. Hartogh, P. Theulé, P.M. Woods, P.M. Woods, R. Hueso, R. Llusar, R. Meier, R. Meier, R. Visser, R. Visser, R. Visser, R.N. Clayton, R.N. Clayton, S. B. Charnley, S. Casassa, S. Casassa, S. Grimme, S. Gulkis, S. Inutsuka, S. N. Milam, S. Wyckoff, S.A. Balbus, S.B. Charnley, S.B. Charnley, S.B. Charnley, S.B. Charnley, S.B. Charnley, S.D. Rodgers, S.E. Dodson-Robinson, T. Albertsson, T. Albertsson, T. Albertsson, T. Bredichin, T. Hama, T. Lee, T. Owen, T.J. Millar, Th. Henning, U. Marboeuf, U. Marboeuf, U. Marboeuf, V. Akimkin, V. Taquet, V. Taquet, V. Wakelam, V. Zubko, W.-H. Ip, W.D. Langer, W.M. Irvine, Y. Aikawa, Y. Aikawa, Y. Aikawa, Y. Aikawa, Y. Aikawa, Y. Aikawa, Y. Alibert, Y. Alibert, Y. Ellinger, Y. Ellinger, Y. Shinnaka, Y.L. Radeva   +227 more
core   +3 more sources

Accretion of dust by chondrules in a MHD-turbulent solar nebula [PDF]

, 2010
(Abridged) Numerical magnetohydrodynamic (MHD) simulations of a turbulent solar nebula are used to study the growth of dust mantles swept up by chondrules. A small neighborhood of the solar nebula is represented by an orbiting patch of gas at a radius of
Armitage, Augusto Carballido, Balbus, Carballido, Carballido, Ciesla, Ciesla, Cuzzi, Cuzzi, Cuzzi, Cuzzi, Fleming, Fromang, Güttler, Hartmann, Hawley, Krot, Leinhardt, Metzler, Morfill, Ormel, Ormel, Rubin, Shakura, Shu, Stone, Stone, Stone, Trigo-Rodrı´guez, Turner, Turner, Weidenschilling, Zsom, Zsom   +33 more
core   +1 more source

Dust photophoretic transport around a T Tauri star: Implications for comets composition [PDF]

, 2016
There is a growing body of evidences for the presence of crystalline material in comets. These crystals are believed to have been annealed in the inner part of the proto-solar nebula, while comets should have been formed in the outer regions.
Cordier, D., Moroni, P. G. Prada, Tognelli, E.   +2 more
core   +4 more sources