Riemannian Acceleration in Oblate Spheroidal Coordinate System
Abstract: The planetary bodies are more of a spheroid than they are a sphere thereby making it necessary to describe motions in a spheroidal coordinate system. Using the oblate spheroidal coordinate system, a more approximate and realistic description of motion in these bodies can be realized. In this paper, we derive the Riemannian acceleration for motion in oblate spheroidal coordinate system using the golden metric tensor in oblate spheroidal coordinates. The Riemannian acceleration in the oblate spheroidal coordinate system reduces to the pure Newtonian acceleration in the limit of c0 and contains post-Newtonian correction terms of all orders of c-2. The result obtained thereby opens the way for further studies and applications of the motion of particles in oblate spheroidal coordinate system.

Received 29 December 2015; accepted 22 February 2016; accepted 25 February 2016

1. Introduction

Most planetary bodies have been assumed to be spherical and consequently, many treatments of motion involving these bodies have been taken into consideration the spherical approximation of the bodies [1] - [3] . However, despite the spherical assumption of planetary bodies, studies have shown that the oblate spheroid is a more approximate description of these bodies [4] - [7] , thus the need for a description of the planetary bodies in terms of the oblate spheroidal coordinate system.

It is worth noting that the description of the planetary bodies mentioned so far have been based on the theory of orthogonal curvilinear coordinates [8] and with foundations on the Euclidean Geometry. However, following the presentation of the work of Riemann in 1854 which laid the foundations for the Riemannian Geometry, there had been considerable interest in the Riemannian Geometry. Consequently, in this paper, we employ the Metric Tensors in oblate spheroidal coordinate system [9] to derive the Riemannian acceleration for the oblate spheroidal coordinate system.

2. Mathematical Formulation

2.1. Oblate Spheroidal Coordinate

In this formulation we have chosen the spheroidal coordinate system based on the approximate representation of the planetary bodies as oblate spheroids. The surface generated by the rotation of an ellipse about its minor axis

is an oblate spheroid. The oblate spheroidal coordinate system is related to the Cartesian coordinate system as follows:

(1)

(2)

(3)

where a is the ellipse’s focal distance and this distance is one-half the ellipse’s foci such that

(4)

Therefore, the differential length of a line element in the oblate spheroidal coordinates is obtained from

(5)

where are the scale factors for the coordinates respectively. Hence, from the theory of orthogonal coordinates [8] [10] , we can write the scale factors explicitly as

(6)

(7)

(8)

Following from Equations (1)-(3), we can define the space time position tensor in oblate spheroidal coordinate system as the set of four labelled quantity as:

(9)

Equation (9) can be written explicitly in terms of the coordinate axes as

(10)

and in Einstein’s coordinates , where t is time coordinate and c is the speed of light in vacuum.

2.2. Metric Tensor

A fundamental quantity in Riemannian coordinate geometry is the metric tensors. Therefore the metric tensor in the oblate spheroidal coordinate system is necessary for the formulation of the Riemannian acceleration in the spheroidal coordinate system. Thus the golden metric tensor in the oblate spheroidal coordinates, , which is a covariant metric tensor of rank 2 [9] is given as follows:

(11)

(12)

(13)

(14)

(15)

where

(16)

is the gravitational scalar potential. From Equations (11)-(15) we can obtain the corresponding contravariant metric tensors, , which is a tensor of rank 2. Therefore, by tensor transformation of Equations (11)-(15), we obtain the corresponding contravariant tensor as:

(17)

(18)

(19)

(20)

(21)

3. Acceleration

With the metric tensors in Equations (11)-(15) and Equations (17)-(21), we can proceed to define another quantity which depends on the metric tensors. This quantity is the Christoffel’s symbols of the second kind or the coefficient of affine connections. The coefficient of affine connection or Christoffels’s symbol of the second kind is the set of labelled quantities, , given by definition [10] [11] as:

(22)

Thus, using Equation (22), and with the metric tensors given by Equations (11)-(15) and Equations (17)-(21), we can obtain all the nonzero terms of the coefficient of affine connections. Hence, after some mathematical simplification, the non-zero terms of Equation (22) is obtained as follows:

(23)

(24)

(25)

(26)

(27)

(28)

(29)

and

(30)

(31)

(32)

(33)

(34)

(35)

(36)

and

(37)

(38)

(39)

(40)

(41)

(42)

(43)

and

(44)

(45)

(46)

(47)

(48)

(49)

(50)

and

(51)

Therefore, the equations given by (23)-(51) denote all the coefficients of affine connection or Christoffel’s symbols of the second kind, where for example, denotes derivative of with respect to the coordinate axes etc.

The first rank tensor, , defined [11] in terms of the Christoffel’s symbols as:

(52)

is called the Riemannian space-time or 4-dimensional “linear acceleration” tensor; and denote one time and two times differentiation with respect to time respectively. However, by tensor analysis [11] , the physical components of the acceleration in oblate spheroidal coordinates, , is given by

(53)

where

(54)

(55)

(56)

(57)

The Equations (54)-(57) are the physically measurable four dimensional acceleration components along the corresponding coordinate axes respectively.

Now, substituting Equations (23)-(51) into Equation (52) and after some mathematical simplification, we can then write Equations (54)-(57) explicitly.

Consequently, Equation (54) for then becomes:

(58)

Equation (55) for then becomes:

(59)

Equation (56) for then becomes:

(60)

and Equation (57) for then becomes:

(61)

where denotes derivative of f with the coordinate axes respectively.

4. Results and Discussion

In this paper, we have derived the Riemannian acceleration for the oblate spheroidal coordinate system. These results are presented in Equations (58)-(61) for the corresponding axes of the oblate coordinate system. The results derived for the linear acceleration vector in Equations (58)-(61) reduce to the pure

Newtonian linear acceleration in the limit of. The results derived here in Equations (58)-(61) contain post Newtonian correction terms of all orders of.

Cite this paper: Omaghali, N. and Howusu, S. (2016) Riemannian Acceleration in Oblate Spheroidal Coordinate System. Journal of Applied Mathematics and Physics, 4, 279-285. doi: 10.4236/jamp.2016.42035.
References

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[7]   Goldreich, P. (1965) Inclination of Satellite Orbits about an Oblate Processing Planet. The Astronomical Journal, 70, 5-9.
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[8]   Morse, P.M. and Feshbach, H. (1953) Methods of Theoretical Physics. McGraw-Hill, New York.

[9]   Howusu, S.X.K. (2013) Riemannian Revolutions in Physics and Mathematics. Jos University Press Ltd., Jos.

[10]   Arfken, G. (1985) Mathematical Methods for Physicists. Academic Press, Orlando.

[11]   Spiegel, M.R. (1974) Theory and Problems of Vector Analysis and Introduction to Tensor Analysis. MC Graw-Hill, New York.

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