This Bromley_readme20210928 was generated on 20210928 by Ben Bromley ------------------- GENERAL INFORMATION ------------------- 1. Title of Dataset Dataset for: From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection 2. Author Information Principal Investigator Contact Information Name: Scott Kenyon Institution: Smithsonian Astrophysical Observatory Address: 60 Garden St, Cambridge, MA 02138 Email: skenyon@cfa.harvard.edu Associate or Co-investigator Contact Information Name: Ben Bromley Institution: University of Utah Address: 115 S 1400 E, SLC, UT 84112 Email: bromley@physics.utah.edu Alternate Contact Information for first author Name: Joan Najita Institution: NSF NOIRLab Address: 950 N. Cherry Ave, Tucson, AZ 85719 Email: joan.najita@noirlab.edu 3. Date of data collection (single date, range, approximate date) 20200601 - 20210928 4. Geographic location of data collection (where was data collected?): NASA NCCS Goddard, MD (supercomputer) 5. Information about funding sources that supported the collection of the data: NASA Emerging Worlds program grant NNX17AE24G -------------------------- SHARING/ACCESS INFORMATION -------------------------- 1. Licenses/restrictions placed on the data: CC BY NC 2. Links to publications that cite or use the data: https://arxiv.org/pdf/2006.13901.pdf Najita, Joan, Kenyon, Scott, and Bromley, Benjamin, 2021. From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection, Astrophysical Journal, in press 3. Links to other publicly accessible locations of the data: N/A 4. Links/relationships to ancillary data sets: N/A 5. Was data derived from another source? no If yes, list source(s): 6. Recommended citation for the data: Najita, Joan, Kenyon, Scott, and Bromley, Ben, 2021. Dataset for: From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection, The Hive: University of Utah Research Data Repository. --------------------- DATA & FILE OVERVIEW --------------------- 1. File List A. Tar file: structure rng1-0NNN.dat.tar │ rng1-0001.dat │ ... | rng1-0148.dat B. rng1-000n: calculations of disks of solids at 30-150 AU, mass = 90 M-Earth n = 1: 100 km solids n = 2: 10 km solids n = 3: 10 km solids n = 4: 100 m solids n = 5: 10 m solids n = 6: 1 m solids n = 7: 10 cm solids n = 8: 1 cm solids C. rng1-00mn: calculations at 36-54 AU, 1 cm + 100 km planetesimals m: denotes total mass of solids n: denotes fraction of initial mass in large planetesimals 47 files total m = 1: 0.01 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 2: 0.03 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 3: 0.10 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 4: 0.30 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 6: f = 1.0e-4 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 5: 1.00 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 6: f = 1.0e-4 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 6: 3.00 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 6: f = 1.0e-4 n = 7: f = 1.0e-5 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 7: 10.0 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 6: f = 1.0e-4 n = 7: f = 1.0e-5 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) D. rng1-01mn: calculations at 60-90 AU, 1 cm + 100 km planetesimals m: denotes total mass of solids n: denotes fraction of initial mass in large planetesimals 50 files total m = 0: 0.01 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 1: 0.1 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 2: 0.5 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 6: f = 1.0e-4 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 4: 1.5 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 6: f = 1.0e-4 n = 7: f = 1.0e-5 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 5: 5.0 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 6: f = 1.0e-4 n = 7: f = 1.0e-5 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 6: 15.0 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 6: f = 1.0e-4 n = 7: f = 1.0e-5 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) m = 7: 45.0 M-Earth n = 1: f = 1.0 (all mass in large planetesimals at t = 0) n = 2: f = 0.3 n = 3: f = 0.1 n = 4: f = 1.0e-2 n = 5: f = 1.0e-3 n = 6: f = 1.0e-4 n = 7: f = 1.0e-5 n = 8: f = 0.0 (all mass in small planetesimals at t = 0) 2. Relationship between files: All files are ASCII text files that contain basic results for the evolution of collections of 1 cm pebbles and 100 km planetesimals in rings at 36-54 AU or at 60-90 AU orbiting a solar-mass star. The calculations run for 10 Gigayears. For variable definitions, see also Kenyon & Bromley, Planetary Science Journal, Volume 1, article 40 and references therein Each file has a header that lists: a) line 1: mass and radius of central star b) line 2: properties of the coagulation grid: # annuli, inner/outer radius in AU, 1 AU c) line 3: min radius of solids, initial small/large radii of solids, fraction of mass in small/large d) line 4: properties of initial size distribution e) line 5: initial eccentricity and inclination of solids f) line 6: initial size distribution (ON/OFF) and fragmentation parameters g) line 7: initial mass in gas/solids in grams h) line 8: column headers time, mass, area, lost mass, mass loss rate, L-dust, r-max (size of largest object), nlarge (# of largest objects), mlarge (mass in largest objects) Following the header are the values from the simulation - logarithm of each value is listed time is in years masses are in grams mass loss rate is in gram per yr dust luminosity (L-dust) is relative to the luminosity of the central star radius is in km The header repeats at end of file 3. Additional related data collected that was not included in the current data package: none 4. Are there multiple versions of the dataset? no If yes, list versions: Name of file that was updated: i. Why was the file updated? ii. When was the file updated? Name of file that was updated: i. Why was the file updated? ii. When was the file updated? -------------------------- METHODOLOGICAL INFORMATION -------------------------- 1. Description of methods used for collection/generation of data: The data were generated with the Orchestra code, a hybrid N-body coaagulation code described in Kenyon, S., and Bromley, B, 2012. Astronomical Journal, 143, 63. A review of the details of this data set is in in Najita, J., Kenyon, S., and Bromley, B., 2021, "From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection," Astrophysical Journal, in press 2. Methods for processing the data: The data are presented as generated by the Orchestra code. 3. Instrument- or software-specific information needed to interpret the data: N/A 4. Standards and calibration information, if appropriate: N/A 5. Environmental/experimental conditions: N/A 6. Describe any quality-assurance procedures performed on the data: The orchestra code has been run through a sseries of validations; see Kenyon, S., and Bromley, B, 2014. Astrophysical Journal, 780, 4 (and references therein). https://iopscience.iop.org/article/10.1088/0004-637X/780/1/4/pdf 7. People involved with sample collection, processing, analysis and/or submission: Author/co-authors ----------------------------------------- DATA-SPECIFIC INFORMATION FOR: all files [format rng1-0###.dat [integer #s] ----------------------------------------- 1. Number of variables: 9 2. Number of cases/rows: for these files the number of rows ranges between between 128 and 3234 3. Variable List A. Time: ltime Description: Log (base 10) of the physical time (years) from start of the simulation of dusty circumstellar disk B. Mass: msolid Description: Log of the total mass in the form of solid material (grams) C. Area: area Description: Log of the area of solids (square-centimeters) D. Mass lost: m-lost Description: Log of cumulative mass lost by depletion processes, e.g., stellar radiation (grams) E. Mass-loss rate: m-dot Description: Log of mass loss rate (grams/year) F. Dust luminosity: l-dust Description: Log of dust luminosity is relative to the luminosity of the central star G. Radius of largest object (planetesimal or protoplanet): r-max Description: The size of the largest object, given as the log of the radius (kilometers) H. Number of large objects: nlarge Description: Log of umber of objects with mass as leasst as much as 10% of the largest object I. Mass in large objects: mlarge Description: Total mass in these large objects, given as a logarithm (grams) 4. Missing data codes: N/A Code/symbol Definition Code/symbol Definition 5. Specialized formats of other abbreviations used N/A