Excitation mechanisms for Jovian seismic modes

被引：24

作者：

Markham, Steve ^{[1
]}

Stevenson, Dave ^{[1
]}

机构：

[1] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA

来源：

ICARUS | 2018年 / 306卷

关键词：

DEDICATED INSTRUMENT; TIDAL DISSIPATION; MOIST CONVECTION; SEISMOLOGY; OSCILLATIONS; INTERIOR; JUPITER; SYMPA;

D O I：

10.1016/j.icarus.2018.02.015

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Recent (2011) results from the Nice Observatory indicate the existence of global seismic modes on Jupiter in the frequency range between 0.7 and 1.5 mHz with amplitudes of tens of cm/s. Currently, the driving force behind these modes is a mystery; the measured amplitudes are many orders of magnitude larger than anticipated based on theory analogous to helioseismology (that is, turbulent convection as a source of stochastic excitation). One of the most promising hypotheses is that these modes are driven by Jovian storms. This work constructs a framework to analytically model the expected equilibrium normal mode amplitudes arising from convective columns in storms. We also place rough constraints on Jupiter's seismic modal quality factor. Using this model, neither meteor strikes, turbulent convection, nor water storms can feasibly excite the order of magnitude of observed amplitudes. Next we speculate about the potential role of rock storms deeper in Jupiter's atmosphere, because the rock storms' expected energy scales make them promising candidates to be the chief source of excitation for Jovian seismic modes, based on simple scaling arguments. We also suggest some general trends in the expected partition of energy between different frequency modes. Finally we supply some commentary on potential applications to gravity, Juno, Cassini and Saturn, and future missions to Uranus and Neptune. (c) 2018 Elsevier Inc. All rights reserved.

引用

页码：200 / 213

页数：14

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