instability of coupled gravity-inertial-rossby waves on a β-plane in solar system atmospheres
Clicks: 118
ID: 183296
2009
Article Quality & Performance Metrics
Overall Quality
Not rated
Combines reader engagement with the AI quality analysis. This
article has not been analysed, so there is no overall score —
reader engagement is measured and shown alongside.
Reader Engagement
Steady Performance
30.0
/100
118 views
15 readers
AI Quality Assessment
Not analyzed
Readership in this journal
SteadyRanked #248 of 484 articles by views in journal of food measurement and characterization
Most read
Least read
Bar heights use a square-root scale. Only the 120 most-read articles are drawn; the journal has 484 in total.
Mint this article as an NFT
Not yet mintedCreate a permanent, verifiable on-chain record of this article on the Scimatic Network. The NFT is held in your Journament account, and you can withdraw it to your own wallet at any time.
5
SUSD
one-off · no wallet required
Abstract
This paper provides an analysis of the combined theory of gravity-inertial-Rossby waves on a β-plane in the Boussinesq
approximation. The wave equation for the system is fifth order in
space and time and demonstrates how gravity-inertial waves on
the one hand are coupled to Rossby waves on the other through the
combined effects of β, the stratification characterized by
the Väisälä-Brunt frequency N, the Coriolis
frequency f at a given latitude, and vertical propagation which
permits buoyancy modes to interact with westward propagating
Rossby waves. The corresponding dispersion equation shows that
the frequency of a westward propagating gravity-inertial wave is
reduced by the coupling, whereas the frequency of a Rossby wave is
increased. If the coupling is sufficiently strong these two modes
coalesce giving rise to an instability. The instability condition
translates into a curve of critical latitude Θc versus
effective equatorial rotational Mach number M, with the region
below this curve exhibiting instability. "Supersonic" fast
rotators are unstable in a narrow band of latitudes around the
equator. For example Θc~12° for Jupiter.
On the other hand slow "subsonic" rotators (e.g. Mercury, Venus
and the Sun's Corona) are unstable at all latitudes except very
close to the poles where the β effect vanishes.
"Transonic" rotators, such as the Earth and Mars, exhibit
instability within latitudes of 34° and
39°, respectively, around the Equator. Similar results
pertain to Oceans. In the case of an Earth's Ocean of depth 4km
say, purely westward propagating waves are unstable up to
26° about the Equator. The nonlinear evolution of this
instability which feeds off rotational energy and gravitational
buoyancy may play an important role in atmospheric dynamics.
| Reference Key |
mckenzie2009annalesinstability
Use this key to autocite in the manuscript while using
SciMatic Manuscript Manager or Thesis Manager
|
|---|---|
| Authors | ;J. F. McKenzie;J. F. McKenzie;J. F. McKenzie |
| Journal | journal of food measurement and characterization |
| Year | 2009 |
| DOI |
10.5194/angeo-27-4221-2009
|
| URL | |
| Keywords |
Citations
No citations found. To add a citation, contact the admin at info@scimatic.org
Comments
No comments yet. Be the first to comment on this article.