Hydrodynamic Simulations of Moonlet-induced Propellers in Saturn's Rings
- One of the biggest successes of the Cassini mission is the detection of small moons (moonlets) embedded in Saturns rings that cause S-shaped density structures in their close vicinity, called propellers. Here, we present isothermal hydrodynamic simulations of moonlet-induced propellers in Saturn's A ring that denote a further development of the original model. We find excellent agreement between these new hydrodynamic and corresponding N-body simulations. Furthermore, the hydrodynamic simulations confirm the predicted scaling laws and the analytical solution for the density in the propeller gaps. Finally, this mean field approach allows us to simulate the pattern of the giant propeller Blériot, which is too large to be modeled by direct N-body simulations. Our results are compared to two stellar occultation observations by the Cassini Ultraviolet Imaging Spectrometer (UVIS), which intersect the propeller Blériot. Best fits to the UVIS optical depth profiles are achieved for a Hill radius of 590 m, which implies a moonlet diameter ofOne of the biggest successes of the Cassini mission is the detection of small moons (moonlets) embedded in Saturns rings that cause S-shaped density structures in their close vicinity, called propellers. Here, we present isothermal hydrodynamic simulations of moonlet-induced propellers in Saturn's A ring that denote a further development of the original model. We find excellent agreement between these new hydrodynamic and corresponding N-body simulations. Furthermore, the hydrodynamic simulations confirm the predicted scaling laws and the analytical solution for the density in the propeller gaps. Finally, this mean field approach allows us to simulate the pattern of the giant propeller Blériot, which is too large to be modeled by direct N-body simulations. Our results are compared to two stellar occultation observations by the Cassini Ultraviolet Imaging Spectrometer (UVIS), which intersect the propeller Blériot. Best fits to the UVIS optical depth profiles are achieved for a Hill radius of 590 m, which implies a moonlet diameter of about 860 m. Furthermore, the model favors a kinematic shear viscosity of the surrounding ring material of ν0 = 340 cm2 s−1, a dispersion velocity in the range of 0.3 cm s−1 < c0 < 1.5 cm s−1, and a fairly high bulk viscosity 7 < ξ0/ν0 < 17. These large transport values might be overestimated by our isothermal ring model and should be reviewed by an extended model including thermal fluctuations.…
Author details: | Martin SeißORCiDGND, Nicole AlbersORCiD, Miodrag SremčevićORCiD, Jürgen SchmidtORCiD, Heikki SaloORCiD, Michael SeilerORCiDGND, Holger HoffmannORCiDGND, Frank SpahnORCiDGND |
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DOI: | https://doi.org/10.3847/1538-3881/aaed44 |
ISSN: | 0004-6256 |
ISSN: | 1538-3881 |
Title of parent work (English): | The astronomical journal |
Subtitle (English): | Application to Bleriot |
Publisher: | IOP Publishing Ltd. |
Place of publishing: | Bristol |
Publication type: | Article |
Language: | English |
Date of first publication: | 2018/12/12 |
Publication year: | 2019 |
Release date: | 2021/05/28 |
Tag: | diffusion; hydrodynamics; planets and satellites: rings |
Volume: | 157 |
Issue: | 1 |
Number of pages: | 11 |
Funding institution: | Deutsches Zentrum fur Luft-und RaumfahrtHelmholtz AssociationGerman Aerospace Centre (DLR) [OH 1401]; Deutsche ForschungsgemeinschaftGerman Research Foundation (DFG) [Sp 384/28-1, Ho5720/1-1]; Cassini project |
Organizational units: | Mathematisch-Naturwissenschaftliche Fakultät / Institut für Physik und Astronomie |
DDC classification: | 5 Naturwissenschaften und Mathematik / 52 Astronomie / 520 Astronomie und zugeordnete Wissenschaften |
Peer review: | Referiert |
Publishing method: | Open Access / Hybrid Open-Access |
License (German): | Creative Commons - Namensnennung, 3.0 Deutschland |