========================================================================== J/ApJS/188/242 Variations on debris disks. II. (Kenyon+, 2010) The following files can be converted to FITS (extension .fit or fit.gz) table*.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/ApJS/188/242 ==========================================================================
drwxr-xr-x 10 cats archive 4096 Jan 29 2012 [Up] drwxr-xr-x 2 cats archive 4096 May 12 09:55 [TAR file] -rw-r--r-- 1 cats archive 467 Jul 29 2010 .message -r--r--r-- 1 cats archive 7704 Jul 29 2010 ReadMe -r--r--r-- 1 cats archive 6000 Jun 17 2010 table11.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 5280 Jun 17 2010 table12.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 4800 Jun 17 2010 table13.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 4200 Jun 17 2010 table14.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 6000 Jun 17 2010 table15.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 5280 Jul 16 2010 table16.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 4800 Jun 17 2010 table17.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 4200 Jun 17 2010 table18.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 4000 Jun 17 2010 table19.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 3520 Jun 17 2010 table20.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 3200 Jun 17 2010 table21.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 2800 Jun 17 2010 table22.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/ApJS/188/242 Variations on debris disks. II. (Kenyon+, 2010) ================================================================================ Variations on debris disks. II. Icy planet formation as a function of the bulk properties and initial sizes of planetesimals. Kenyon S.J., Bromley B.C. <Astrophys. J. Suppl. Ser., 188, 242-279 (2010)> =2010ApJS..188..242K ================================================================================ ADC_Keywords: Models, evolutionary Keywords: circumstellar matter - planetary systems - protoplanetary disks - planets and satellites: formation - stars: formation - zodiacal dust Abstract: We describe comprehensive calculations of the formation of icy planets and debris disks at 30-150AU around 1-3M_sun_ stars. Disks composed of large, strong planetesimals produce more massive planets than disks composed of small, weak planetesimals. The maximum radius of icy planets ranges from 1500km to 11500km. The formation rate of 1000km objects-"Plutos"-is a useful proxy for the efficiency of icy planet formation. Plutos form more efficiently in massive disks, in disks with small planetesimals, and in disks with a range of planetesimal sizes. Although Plutos form throughout massive disks, Pluto production is usually concentrated in the inner disk. Despite the large number of Plutos produced in many calculations, icy planet formation is inefficient. At the end of the main sequence lifetime of the central star, Plutos contain less than 10% of the initial mass in solid material. This conclusion is independent of the initial mass in the disk or the properties of the planetesimals. Debris disk formation coincides with the formation of planetary systems containing Plutos. As Plutos form, they stir leftover planetesimals to large velocities. A cascade of collisions then grinds the leftovers to dust, forming an observable debris disk. In disks with small (< 1-10km) planetesimals, collisional cascades produce luminous debris disks with maximum luminosity 10-2 times the stellar luminosity. Disks with larger planetesimals produce debris disks with maximum luminosity 5x10^-4^ (10km) to 5x10^-5^ (100km) times the stellar luminosity. Following peak luminosity, the evolution of the debris disk emission is roughly a power law, fproptot^-n^ with n 0.6-0.8. Observations of debris disks around A-type and G-type stars strongly favor models with small planetesimals. In these models, our predictions for the time evolution and detection frequency of debris disks agree with published observations. We suggest several critical observations that can test key features of our calculations.
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