Theories of Polar Motion from Tisserand to Poincaré (1890 – 1910)

2000 ◽  
Vol 178 ◽  
pp. 41-66 ◽  
Author(s):  
P. Melchior
Keyword(s):  
Polar Motion ◽  
Scientific Community ◽  
Circular Motion ◽  
Computing Power ◽  
The Earth ◽  
Fixed Pole ◽  
One Year ◽  
Elliptical Motion ◽  
The Impact ◽  
Chandler Period

AbstractThe discovery by Seth C. Chandler (1891) that the motion of the pole (the reality of which had been established by K.F. Küstner and by the simultaneous latitude observations at Honolulu and Berlin by German astronomers) resulted from two components i.e. a free circular motion with a period of 427 days and a forced elliptical motion with a period of 365.25 days, raised considerable interest in the scientific community of astronomers and geophysicists.The celebrated Mécanique Céleste of Tisserand (1890) had been published just one year before at a time when doubts still persisted and arguments could be presented in favor of the fixed pole. Starting with Tisserand’s arguments, we describe in this paper the impact of the successive contributions by A. Greenhill, S. Newcomb, Th. Sloudsky, S. Hough, G. Herglotz, A. Love, J. Larmor and H. Poincaré to the solution of the problems raised by the Chandler period.The lines of reasoning taken by these eminent scientists were rigorously correct so that, after about one hundred years, contemporary researchers, who benefit from a far better knowledge of the inner structure of the Earth and are able to take advantage of modern computing power, do not contradict any of their conclusions and instead refine them with an accuracy which was not imaginable one century ago.

scholarly journals Excitation of the Chandler Wobble

2000 ◽  
Vol 178 ◽  
pp. 455-462
Author(s):  
N.S. Sidorenkov
Keyword(s):  
Polar Motion ◽  
Southern Oscillation ◽  
World Ocean ◽  
Noise Spectrum ◽  
Chandler Wobble ◽  
The Earth ◽  
The Pacific ◽  
And Shifts ◽  
Chandler Period ◽  
Earth’S Inertia Tensor

AbstractThe redistribution of air and water masses between the Pacific and Indian oceans during the El Niño/Southern oscillation (ENSO) changes the components of the Earth’s inertia tensor and shifts the position of the pole of the Earth’s rotation. The spectrum of the ENSO has components with periods of about 6, 3.6, 2.8, and 2.4 years. These periods are all the multiples of the Chandler period T = 1.2 yr. and the principal period of nutation 18.6 yr. A nonlinear model for the Chandler polar motion has been constructed based on this empirical fact. In this model, the ENSO excites the Chandler polar motion by acting on the Earth at the frequencies of combinative resonance. At the same time, the Chandler polar motion induces a polar tide in the atmosphere and the World Ocean, which orders the ENSO. As a result, the dominant components in the noise spectrum of the ENSO are those with the periods indicated above.

scholarly journals Analysis of the Chandler Period of Polar Coordinates Calculated by the Orlov Method

1972 ◽  
Vol 48 ◽  
pp. 43-45 ◽  
Author(s):  
E. Proverbio ◽  
F. Carta ◽  
F. Mazzoleni
Keyword(s):  
Polar Motion ◽  
Homogeneous System ◽  
Time Variable ◽  
Polar Coordinates ◽  
Variable Model ◽  
Chandler Period

The coordinates x and y of the pole related to mean pole of the epoch in the period 1900–1962 for the ILS station were calculated utilising the method proposed by Orlov (1955). The values of the latitudes are those reduced in the homogeneous system of Carnera-Cecchini by Proverbio et al. (1969). The values of the amplitudes and periods of the polar motion were calculated. The comparison of the data seems to confirm a correlation between the amplitudes and periods of Chandler motion, that is the validity of the time-variable model suggested by Melchior (1949) and other authors.

scholarly journals On the Chandler periodicity (Polar Motion, LOD and Climate)

2000 ◽  
Vol 178 ◽  
pp. 397-402
Author(s):  
F. Buffa ◽  
A. Poma
Keyword(s):  
Time Series ◽  
Polar Motion ◽  
Superconducting Gravimeter ◽  
Spin Axis ◽  
Rainfall Time Series ◽  
Observation Level ◽  
Motion Data ◽  
The Earth ◽  
Chandler Period ◽  
Free Nutation

AbstractThe 14-month Chandler period is associated with the free nutation of the Earth about its spin axis. The observed value of the Chandler period comes usually from the analysis of astronomical series of polar motion data as well as from superconducting gravimeter measurements. At the observation level a periodicity of about 420–440 days also was noticed in microseismic activities. Recently we found evidence of a signal with period similar to the Chandler one in the Sardinia rainfall time series.

scholarly journals Polar Motion through 1977 from Doppler Satellite Observations

1979 ◽  
Vol 82 ◽  
pp. 263-278 ◽  
Author(s):  
Claus Oesterwinter
Keyword(s):  
Standard Error ◽  
Polar Motion ◽  
Daily Basis ◽  
Pole Position ◽  
Satellite Observations ◽  
Doppler Data ◽  
Chandler Period

Doppler observations of Navy Navigation Satellites have been used to compute pole positions on a daily basis since 1969. Limited results exist for the period 1964 to 1969. Based on Doppler observations from four or five satellites, the standard error for a five-day mean pole position is less than 20 cm. Comparisons are made between BIH, IPMS and ILS results and those obtained from Doppler. It is shown that the six years of reliable Doppler data since 1972 contribute little in finding the Chandler period. Using observations from the three astronomical sources over 12 years yields a Chandler period of 432.0 ± 0.2 days.

scholarly journals Dissipation and Ellipticity of the Chandler Wobble

2000 ◽  
Vol 178 ◽  
pp. 473-480
Author(s):  
Yaozhong Zhu ◽  
Buxi Gao
Keyword(s):  
Energy Dissipation ◽  
Opposite Direction ◽  
Polar Motion ◽  
Semimajor Axis ◽  
Liquid Core ◽  
Chandler Wobble ◽  
Motion Data ◽  
Pole Tide ◽  
Chandler Period ◽  
Theoretical Results

AbstractThe Chandler wobble, one of the main feature of the Earth’s polar motion, is related to the properties of the mantle and liquid core as well as the mobility of the oceans. The equilibrium pole tide and mantle anelasticity both lengthen the Chandler period, moreover, the former imposes a slight ellipticity on the pole path, and the latter is responsible for the wobble energy dissipation. On the basis of the perturbation principles, we derive the theoretical Qω of the Chandler wobble, assuming that the wobble energy is totally dissipated within the mantle. The theoretical ellipticity and orientation of the semimajor axis of the Chandler wobble path for an anelastic Earth are given. Compared with the results for the elastic Earth, the effect of mantle anelasticity does not change the wobble ellipticity significantly, but slightly changes the orientation of the semimajor axis in the opposite direction. This paper has also proved that the effect of the Earth’s 3-axis feature on the wobble ellipticity is only about 19% of that of the equilibrium pole tide. Analysis of the polar motion data obtained by using modern geodetic techniques shows that the observed ellipticity and orientation of the semimajor axis agree with the theoretical results. We can deduce that the pole tide in the globe should be close to equilibrium.

scholarly journals The Study of the Structure of 142-Year Series of Pole Coordinates

1990 ◽  
Vol 141 ◽  
pp. 157-159
Author(s):  
L.V. Rykhlova ◽  
G.S. Kurbasova
Keyword(s):  
Initial Data ◽  
Best Approximation ◽  
The Best Approximation ◽  
Chandler Period

The 142-year series of pole coordinates in the system of mean pole of epoch of observation are used for the investigation of the Chandler period. The method of the best approximation of the initial data with the step of 1.5 years by means of quasi-polynomials is used.

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