Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:0806.1521)
· References in the article
· Citations to the Article (10) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (1)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Assembling the Building Blocks of Giant Planets Around Intermediate-Mass Stars
Authors:
Kretke, K. A.; Lin, D. N. C.; Garaud, P.; Turner, N. J.
Affiliation:
AA(Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA ), AB(Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064, USA ; Kavli Institute of Astronomy and Astrophysics, Peking University, Beijing, China ), AC(Department of Applied Mathematics and Statistics, Baskin School of Engineering, University of California, Santa Cruz, CA 95064, USA ), AD(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA)
Publication:
The Astrophysical Journal, Volume 690, Issue 1, pp. 407-415 (2009). (ApJ Homepage)
Publication Date:
01/2009
Origin:
IOP
ApJ Keywords:
planetary systems: formation, planetary systems: protoplanetary disks
DOI:
10.1088/0004-637X/690/1/407
Bibliographic Code:
2009ApJ...690..407K

Abstract

We examine a physical process that leads to the efficient formation of gas giant planets around intermediate-mass stars. In the gaseous protoplanetary disks surrounding rapidly accreting intermediate-mass stars, we show that the midplane temperature (heated primarily by turbulent dissipation) can reach gsim 1000 K out to 1 AU. The thermal ionization of this hot gas couples the disk to the magnetic field, allowing the magnetorotational instability (MRI) to generate turbulence and transport angular momentum. Further from the central star the ionization fraction decreases, decoupling the disk from the magnetic field and reducing the efficiency of angular momentum transport. As the disk evolves toward a quasi-steady state, a local maximum in the surface density and in the midplane pressure both develop at the inner edge of the MRI-dead zone, trapping inwardly migrating solid bodies. Small particles accumulate and coagulate into planetesimals which grow rapidly until they reach isolation mass. In contrast to the situation around solar-type stars, we show that the isolation mass for cores at this critical radius around the more-massive stars is large enough to promote the accretion of significant amounts of gas prior to disk depletion. Through this process, we anticipate a prolific production of gas giants at ~1 AU around intermediate-mass stars.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints