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Historical Background

The Earth's polar motion has been observed for over a hundred years, initially by astrometric and in modern times by space geodetic techniques. The polar motion excitation function derived from these observations shows a generally broad-band structure, but with certain prominent signals superimposed: a more-or-less secular drift largely attributed to the present-day post-glacial rebound, a 30-year Markowitz wobble whose origin remains mysterious, and the very notable annual wobble of obvious meteorological origin.

In addition, the observed polar motion has a strong Chandler wobble component with a time-varying amplitude comparable to that of the annual wobble. Although the Chandler wobble is a natural free mode, it still needs continual excitation to maintain its observed amplitude. Despite many studies, the Chandler wobble's excitation sources have remained elusive to date, although atmospheric angular momentum variations, perhaps together with oceanic variations, may prove to be largely responsible for its excitation.

Historically, another notable candidate excitation source for the Chandler wobble was seismic dislocation; a first proposal was made as early as Milne (1907), soon after the annual and Chandler wobbles were identified. Cecchini (1928) later noted some correlation between the large polar motion and the high seismicity during 1900-1908. Similar correlations have been alluded to in subsequent reports, such as Runcorn (1970), Pines and Shaham (1973), Press and Briggs (1975), Kanamori (1976).
However, to establish an unequivocal relationship between seismic excitation and the observed polar motion, one needs to be able to compute quantitatively how much an earthquake can excite polar motion by altering the Earth's inertia tensor. In their milestone geophysical monograph, Munk and MacDonald (1960) briefly treated the problem. They used a simplistic local block-dislocation model for an earthquake, and quickly dismissed the importance of earthquakes in polar motion excitation, even for the largest earthquakes.

Then came the great 1964 Alaskan earthquake, which provided new, fundamental insight into the displacement field of an earthquake: Based on a strainmeter record in Hawaii, Press (1965) announced that a static displacement was recorded at teleseismic distances several thousand kilometers from the epicenter. That prompted a series of investigations of seismic excitation of polar motion: Mansinha and Smylie (1967), Smylie and Mansinha (1968; 1971), Mansinha et al. (1970; 1979), Ben-Menahem and Israel (1970), Israel et al. (1973), Israel and Ben-Menahem (1975), Rice and Chinnery (1972), Dahlen (1971; 1973), O'Connell and Dziewonski (1976), Smith (1977). Unfortunately the search for signatures left by large earthquakes (e.g., the great 1960 Chilean event and the 1964 Alaskan event) in polar motion was essentially inconclusive: the quality of the polar motion data at the time was insufficient for that purpose both in accuracy and temporal resolution.

A revival of interest in the problem appeared during the latter half of the 1980s, largely because of advances in polar motion measurement techniques, but also owing to the availability of the Harvard centroid moment tensor (CMT) catalog of all major earthquakes (see below). Using Dahlen's (1973) formula on the thousands of earthquakes listed in the catalog, Souriau and Cazenave (1985) and Gross (1986) computed time series of seismic excitation of polar motion. They concluded that the earthquakes since 1977 were simply too small to produce any appreciable signature in polar motion, with the cumulative seismic excitation power being orders of magnitude smaller than that observed.

The next development was by Chao and Gross (1987) who again computed the seismic excitation of polar motion for all events listed in the CMT catalog, but using the normal-mode summation scheme of Gilbert (1970). Their method has since remained a most efficient way of computing the seismic excitation of not only polar motion, but also of other important geodynamic parameters such as gravitational field changes. Furthermore, Chao and Gross (1995) and Chao et al. (1995) extended the formulation to compute earthquake-induced changes in rotational energy and gravitational energy, respectively. These papers and later Chao et al. (1996) have updated, and in fact strengthened, the results of Chao and Gross (1987) who found many earthquake-induced phenomena having intriguing geodynamical implications, listed as (4)-(6) above.

It should be stressed that all these studies only pertain to the coseismic effects, that is, to the effect due to the elastic dislocation that happens within, say, an hour following the initial rupture of the fault. The inelastic pre- or post-seismic movements that are often associated with large earthquakes on timescales of months to years have been studied based on rheological modeling (e.g., Dragoni et al., 1983; Sabadini et al.,1984; Soldati and Spada, 1999) . These effects typically augment the coseismic ones by a factor depending on the source mechanism and mantle rheology.