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  • Dataset for: A Pluto-Charon Concerto: An Impact on Charon as the Origin of the Small Satellites

    Description:
    We consider a scenario where the small satellites of Pluto and Charon grew within a disk of debris from an impact between Charon and a trans-Neptunian Object (TNO). After Charon’s orbital motion boosts the debris into a disk-like structure, rapid orbital damping of meter-size or smaller objects is essential to prevent the subsequent re-accretion or dynamical ejection by the binary. From analytical estimates and simulations of disk evolution, we estimate an impactor radius of 30–100 km; smaller (larger) radii apply to an oblique (direct) impact. Although collisions between large TNOs and Charon are unlikely today, they were relatively common within the first 0.1–1 Gyr of the solar system. Compared to models where the small satellites agglomerate in the debris left over by the giant impact that produced the Pluto-Charon binary planet, satellite formation from a later impact on Charon avoids the destabilizing resonances that sweep past the satellites during the early orbital expansion of the binary.
    Subject:
    Astronomy and Astrophysics
    Creator:
    Kenyon, Scott and Bromley, Ben
    Owner:
    BENJAMIN BROMLEY
    Language:
    English
    Date Uploaded:
    07/07/2020
    Date Modified:
    07/10/2020
    Date Created:
    201911 - 202004
    Identifier:
    https://doi.org/10.7278/S50D4AKFQZFC

  • Data for: A Pluto-Charon Concerto II. Formation of a Circumbinary Disk of Debris After the Giant Impact

    Description:
    Using a suite of numerical calculations, we consider the long-term evolution of circumbinary debris from the Pluto--Charon giant impact. Initially, these solids have large eccentricity and pericenters near Charon's orbit. On time scales of 100--1000 yr, dynamical interactions with Pluto and Charon lead to the ejection of most solids from the system. As the dynamics moves particles away from the barycenter, collisional damping reduces the orbital eccentricity of many particles. These solids populate a circumbinary disk in the Pluto-Charon orbital plane; a large fraction of this material lies within a `satellite zone' that encompasses the orbits of Styx, Nix, Kerberos, and Hydra. Compared to the narrow rings generated from the debris of a collision between a trans-Neptunian object (TNO) and Charon, disks produced after the giant impact are much more extended and may be a less promising option for producing small circumbinary satellites.
    Subject:
    Astronomy
    Creator:
    Bromley, Benjamin and Kenyon, Scott
    Owner:
    BENJAMIN BROMLEY
    Language:
    English
    Date Uploaded:
    02/03/2021
    Date Modified:
    12/09/2021
    Date Created:
    20191115 to 20200220
    Resource Type:
    Dataset
    Identifier:
    https://doi.org/10.7278/S50DSSMBHHXN

  • A Pluto-Charon Sonata: Growth of Charon from a Circum-Pluto Ring of Debris

    Creator:
    Bromley, Benjamin and Kenyon, Scott
    Owner:
    BENJAMIN BROMLEY
    Language:
    English
    Date Uploaded:
    07/26/2019
    Date Modified:
    12/09/2021
    Resource Type:
    Dataset and Software or Program Code
    Identifier:
    https://doi.org/10.7278/S50D-EFCY-ZC00

  • Datasets for: A Pluto-Charon Sonata: Dynamical Limits on the Masses of the Small Satellites

    Description:
    -------------------------- METHODOLOGICAL INFORMATION -------------------------- 1. Description of methods used for collection/generation of data: The data were generated by computer simulations using the C++ code "Orchestra", a proprietary hybrid code that follows the dynamical evolution of solids and gas orbiting a central object. Algorithms in the code are described in the following papers (author names abbreviated to B for Bromley, K for Kenyon, and L for Jane X Luu along with a year for publication date, AJ = Astronomical Journal, ApJ = Astrophysical Journal, S=Supplement): KL1998, AJ 115:2136; KL1999, AJ 118:1101; KB2001,AJ 121:538; KB2002,AJ 123:1757; KB2004, AJ 127:513; BK2006, AJ 131:2737; KB2006, AJ 131:1837; KB2008, ApJS 179:451; KB2010, ApJS 188:242; BK2011, ApJ 731:101; KB2012, AJ 143:63; KB2014, AJ 147:8. Initial conditions for these simulations described in the published paper. 2. Methods for processing the data: Various C and fortran programs are used to analyze the data for the calculations. Several C programs needed to extract information from the computer generated binary output files are included with the dataset. The C programs include basic summaries of the structure of the data files and the usage to extract data from each binary file. 3. Instrument- or software-specific information needed to interpret the data: Appropriate software is included in directory. 4. Standards and calibration information, if appropriate: none 5. Environmental/experimental conditions: all calculations were run on the NASA discover cluster 6. Describe any quality-assurance procedures performed on the data: Aside from tests summarized in the papers described in item 1, test calculations are summarized in the Appendix of each paper and compared to an appropriate benchmark. 7. People involved with sample collection, processing, analysis and/or submission: Scott Kenyon and Ben Bromley and --------------------- DATA & FILE OVERVIEW --------------------- Files summarized in items 1-8 are binary output files from n-body simulations as described in Kenyon & Bromley, "A Pluto-Charon Sonata: Dynamical Limits on fate Masses of the Small Satellites" (2019, Astronomical Journal). Files described in item 9 are ascii txt. The C programs in items 10, 11, and 12 provide different ways to access the binary output. Each C program describes the architecture of the binary files. 1. pcs2-0mmm-nnn[a-z] files: heavy satellites, mmm = 100 x mass factor for all satellites, nnn = number of Symplectic steps per PC orbit, a-z = version 2. pcs2-1mmm-nnn[a-z] files: light satellites, mmm = 100 x mass factor for all satellites, nnn = number of Symplectic steps per PC orbit, a-z = version 3. pcs2-2mmm-nnn[a-z] files: light satellites with 2x nominal mass of Styx & Kerberos, mmm = 100 x mass factor for all satellites, nnn = number of Symplectic steps per PC orbit, a-z = version 4. pcs2-3mmm: heavy satellites, 40 Symplectic steps per PC orbit, mmm = 100 x mass factor for Nix only 5. pcs2-4mmm: heavy satellites, 40 Symplectic steps per PC orbit, mmm = 100 x mass factor for Kerberos only 6. pcs2-5mmm: heavy satellites, 40 Symplectic steps per PC orbit, mmm = 100 x mass factor for Hydra only 7. pcs2-6mmm light satellites, 40 Symplectic steps per PC orbit, mmm = 100 x mass factor for Nix only 8. pcs2-7mmm: light satellites, 40 Symplectic steps per PC orbit, mmm = 100 x mass factor for Hydra only 9. pcs2-n000.dat: summary of lifetimes for binary files in each archive 10. lifetime.c: summarizes lifetime and mass factor for binary file usage example: "lifetime pcs2-6110" 11. summary.c: generates basic summary of timesteps in a binary file usage example: "summary pcs1-0013d" 12. extrxyz.c: extracts (x,y,z) for N satellites and outputs (x,y,z) usage example: "extr6d pcs1-6110 6" will output (x,y,z) for SNKH 3. Additional related data collected that was not included in the current data package: There are other binary output files not included in this archive. 4. Are there multiple versions of the dataset? no
    Subject:
    Astrophysics
    Creator:
    Bromley, Benjamin and Kenyon, Scott
    Depositor:
    BRIAN MCBRIDE
    Owner:
    BENJAMIN BROMLEY
    Language:
    English
    Date Uploaded:
    07/11/2019
    Date Modified:
    04/04/2022
    Date Created:
    2018-2019
    Resource Type:
    Dataset
    Identifier:
    https://doi.org/10.7278/S50D-HAJT-E0G0

  • Dataset for: From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection

    Description:
    The similar orbital distances and incidence rates of debris disks and the prominent rings observed in protoplanetary disks suggest a potential connection between these structures. We explore this connection with new calculations that follow the evolution of rings of pebbles and planetesimals as they grow into planets and generate dusty debris. Depending on the initial solid mass and planetesimal formation efficiency, the calculations predict diverse outcomes for the resulting planet masses and accompanying debris signature. When compared with debris disk incidence rates as a function of luminosity and time, the model results indicate that the known population of bright cold debris disks can be explained by rings of solids with the (high) initial masses inferred for protoplanetary disk rings and modest planetesimal formation efficiencies that are consistent with current theories of planetesimal formation. These results support the possibility that large protoplanetary disk rings evolve into the known cold debris disks. The inferred strong evolutionary connection between protoplanetary disks with large rings and mature stars with cold debris disks implies that the remaining majority population of low-mass stars with compact protoplanetary disks leave behind only modest masses of residual solids at large radii and evolve primarily into mature stars without detectable debris beyond 30 au. The approach outlined here illustrates how combining observations with detailed evolutionary models of solids strongly constrains the global evolution of disk solids and underlying physical parameters such as the efficiency of planetesimal formation and the possible existence of invisible reservoirs of solids in protoplanetary disks.
    Keyword:
    model, low-mass stars, debris disks, planetesimals, protoplanetary disks, ring of pebbles, and planet formation
    Subject:
    Astronomy
    Creator:
    Kenyon, Scott, Najita, Joan, and Bromley, Ben
    Owner:
    BENJAMIN BROMLEY
    Based Near Label Tesim:
    Goddard, Maryland, United States
    Language:
    English
    Date Uploaded:
    10/01/2021
    Date Modified:
    12/06/2023
    Date Created:
    2020-06-01 to 2021-09-28
    License:
    CC BY NC - Allows others to use and share your data non-commercially and with attribution.
    Resource Type:
    Dataset