Mass Distribution and Planet Formation in the Solar Nebula

By S. Desch. 2007

182 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/054e675d459212463f2ec9770f858eaaf3c4505b

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In Astronomy and Astrophysics

Citations in the corpus

The Birth Environment of the Solar System (2010, background): “Since planets can migrate, the starting surface density of the nebula is subject to further uncertainty (compare Desch 2007 and Crida 2009).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, background): “…the MMSN: the abundances of key elements in current planet compositions, the arbitrary assignment of annular bins to smear out augmented masses, and the implicit assumption that the nebular material was stationary throughout its evolution, to name a few (see Cameron 1988; Desch 2007; Crida 2009).”
SOLAR MODELS WITH ACCRETION. I. APPLICATION TO THE SOLAR ABUNDANCE PROBLEM (2011, background): “Given that models of massive disks with steep density profiles lead to substantial (Desch 2007) evaporation, 0.06 M⊙ is probably a safe upper bound on the amount of mass that could have been chemically processed in the protoplanetary disk and later accreted onto the Sun.”
Protoplanetary Disks and Their Evolution (2011, background): “The extrapolated surface density profile, which is an observable for resolved disks, has an approximate power law form, Σ ∝ r−3/2, although more sophisti- cated fits based on viscous disk evolution and planet migration models can be made (Davis 2005, Desch 2007).”
WIND-DRIVEN ACCRETION IN PROTOPLANETARY DISKS. I. SUPPRESSION OF THE MAGNETOROTATIONAL INSTABILITY AND LAUNCHING OF THE MAGNETOCENTRIFUGAL WIND (2013, background): “The MMSN surface density serves as an initial guess and is likely on the lower end, while much more massive inner disks are also speculated (e.g., Desch 2007).”
Planetesimal formation by sweep-up: how the bouncing barrier can be beneficial to growth (2012, background): “It however excludes the effect of planetary migration and radial drift of dust grains, and the real initial disk profile might have been much different (Desch 2007).”
A dual-frequency sub-arcsecond study of proto-planetary disks at mm wavelengths: first evidence for radial variations of the dust properties (2011, methodology): “The solution proposed by Desch (2007) (see Appendix E) for the Solar Nebula is a steady-state solution, which allows for sufficient time (few Myr) for the giant planets to reach isolation mass.”
Breaking through: The effects of a velocity distribution on barriers to dust growth (2012, background): “It is now well-known known that the gas and dust mass of the solar nebula might have been much higher (Desch 2007), which would increase the coagulation rates and the particle size at the fragmentation barrier (Birnstiel et al. 2011).”
EVIDENCE OF FAST PEBBLE GROWTH NEAR CONDENSATION FRONTS IN THE HL TAU PROTOPLANETARY DISK (2015, background): “The frost lines of abundant ices have long been thought to be important for planet formation, in part because the extra material provided by condensation can significantly enhance the local mass surface density of solids in the disk (Hayashi 1981; Stevenson & Lunine 1988; Desch 2007).”