Results 111 to 120 of about 15,247 (235)

Mini-Oort clouds: compact isotropic planetesimal clouds from planet–planet scattering [PDF]

, 2012
Sean N. Raymond, Philip J. Armitage
openalex   +1 more source

Porosity models for pre-planetesimals: modified P-α like models and the effect of dissipated energy [PDF]

, 2010
S. E. Arena, R. Speith
openalex   +1 more source

Argon in β Pictoris–Entrapment and Release of Volatile in Disks

The Astrophysical Journal
Chemical compositions of planets reveal much about their formation environments. Such information is well sought-after in studies of solar system bodies and extrasolar ones.
Yanqin Wu, Kadin Worthen, Alexis Brandeker, Christine Chen   +3 more
doaj   +1 more source

Long-term, multiwavelength light curves of ultra-cool dwarfs: II. The evolving light curves of the T2. 5 SIMP 0136 & the uncorrelated light curves of the M9 TVLM 513 [PDF]

, 2016
We present multiwavelength, multi-telescope, ground-based follow-up photometry of the white dwarf WD 1145+017, that has recently been suggested to be orbited by up to six or more, short-period, low- mass, disintegrating planetesimals.
Croll, B., Dalba, P. A., Han, E., Lichtman, J., Muirhead, P. S., Radigan, J.   +5 more
core   +1 more source

Shock-generating Planetesimals Perturbed by a Giant Planet in a Gas Disk [PDF]

, 2019
Makiko Nagasawa, Kyoko K. Tanaka, Hidekazu Tanaka, Hideko Nomura, T. Nakamoto, Hitoshi Miura   +5 more
openalex   +1 more source

Vom Staubkorn zum Planetesimal [PDF]

Physik in unserer Zeit, 2019
ZusammenfassungDurch astronomische Beobachtungen, numerische Simulationen und Laborexperimente sind wir erstmals in der Lage, ein in sich geschlossenes Bild der Entstehung der ersten größeren Körper in jungen Planetensystemen zu zeichnen. Mikroskopisch kleine Staubpartikel verklumpen durch haftende Stöße zu millimeter‐ bis zentimetergroßen Agglomeraten.
openaire   +1 more source

Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall

The Astrophysical Journal
There is growing evidence that planet formation begins early, within the ≲1 Myr Class 0/I phase, when infall dominates disk dynamics. Our goal is to determine if Class 0/I disks reach the conditions needed to form planetesimals (∼100 km planet building ...
Daniel Carrera, Abigail Davenport, Jacob B. Simon, Hans Baehr, Til Birnstiel, Cassandra Hall, David Rea, Sebastian Markus Stammler   +7 more
doaj   +1 more source

Gas giant formation with small cores triggered by envelope pollution by icy planetesimals [PDF]

, 2011
Y. Hori, M. Ikoma
openalex   +1 more source

Origins of Mercury’s Big Heart of Iron: Exploring Pathways to Form High Core Mass Fraction Planets via N-body Simulations

The Astrophysical Journal
Mercury’s core mass fraction (CMF) is 0.7, more than double that of the other rocky planets in the solar system, which have CMFs of 0.3 or lower. The origin of Mercury’s large, iron-rich core remains unknown. Adding to this mystery, an elusive population
Haniyeh Tajer, Ji Wang, Anna C. Childs, Noah Ferich, Tiger Lu, Hanno Rein   +5 more
doaj   +1 more source

FORMING PLANETESIMALS BY GRAVITATIONAL INSTABILITY. I. THE ROLE OF THE RICHARDSON NUMBER IN TRIGGERING THE KELVIN-HELMHOLTZ INSTABILITY [PDF]

, 2010
Aaron T. Lee, Eugene Chiang, Xylar Asay-Davis, Joseph Barranco   +3 more
openalex   +1 more source