Capture and evolution of dust in planetary mean-motion resonances: A fast, semi-analytic method for generating resonantly trapped disk images
Entity
UAM. Departamento de Física TeóricaPublisher
Oxford University Press on behalf of the Royal Astronomical SocietyDate
2015-06-09Citation
10.1093/mnras/stv045
Monthly Notices of Royal Astronomical Society 448.1 (2015): 684-702
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1093/mnras/stv045Funded by
AS and MW are supported by the European Union through ERC grant number 279973, AJM acknowledges support from Spanish grant AYA 2010/20630, grant number KAW 2012.0150 from the Knut and Alice Wallenberg foundation, and the Swedish Research Council (grant 2011-3991)Project
Gobierno de España. AYA 2010/20630Editor's Version
http://dx.doi.org/10.1093/mnras/stv045Subjects
Dust; Planetary; Resonances; N-body simulations; Zodiacal cloud; FísicaNote
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reservedRights
© 2015 The AuthorsAbstract
Dust grains migrating under Poynting-Robertson drag may be trapped in mean-motion resonances with planets. Such resonantly trapped grains are observed in the Solar system. In extrasolar systems, the exozodiacal light produced by dust grains is expected to be a major obstacle to future missions attempting to directly image terrestrial planets. The patterns made by resonantly trapped dust, however, can be used to infer the presence of planets, and the properties of those planets, if the capture and evolution of the grains can be modelled. This has been done with N-body methods, but such methods are computationally expensive, limiting their usefulness when considering large, slowly evolving grains, and for extrasolar systems with unknown planets and parent bodies, where the possible parameter space for investigation is large. In this work, we present a semi-analytic method for calculating the capture and evolution of dust grains in resonance, which can be orders of magnitude faster than N-body methods. We calibrate the model against N-body simulations, finding excellent agreement for Earth to Neptune mass planets, for a variety of grain sizes, initial eccentricities, and initial semimajor axes. We then apply the model to observations of dust resonantly trapped by the Earth. We find that resonantly trapped, asteroidally produced grains naturally produce the 'trailing blob' structure in the zodiacal cloud, while to match the intensity of the blob, most of the cloud must be composed of cometary grains, which owing to their high eccentricity are not captured, but produce a smooth disc
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Google Scholar:Shannon, Andrew
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Mustill, Alexander J.
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Wyatt, Mark
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