# Spherical Geometry

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## spherical geometry

[′sfir·ə·kəl je′äm·ə·trē]*The Great Soviet Encyclopedia*(1979). It might be outdated or ideologically biased.

## Spherical Geometry

the mathematical discipline that studies geometric figures on a sphere, just as plane geometry studies geometric figures in the plane.

Every plane section of a sphere is a circle. If the plane passes through the center *O* of the sphere, the resulting section is called a great circle. Only one great circle can be drawn through two points *A* and *B* on a sphere (Figure 1,1), unless the points are antipodal. The great circles of a sphere are geodesies, and thus play in spherical geometry a role analogous to that of straight lines in plane geometry. Whereas, however, any line segment is the shortest distance between its end points, only the shorter, or minor, arc of a great circle determined by two nonantipodal points has this property. Spherical geometry differs from plane geometry in many other respects as well. For example, there are no parallel geodesies in spherical geometry, since two great circles always intersect; in fact, they always intersect at two points.

The length of the segment *AB* on a sphere—that is, the length of the arc *AmB* (Figure 1,1) of a great circle—can be measured by means of the angle *AOB*, which is proportional to the length of the arc. The measure of the angle *ABC* (Figure 1,2) formed on a sphere by the intersection of two great circles is the angle *A’BC’* between the tangents to the corresponding arcs at the point of intersection *B* and is thus equal to the measure of the dihedral angle formed by the planes *OBA* and *OBC*.

Four lunes are formed by the intersection of two great circles on a sphere (Figure 1,3). A lune is determined by specifying its angle. The area of a lune is given by the formula *S* = 2*R*^{2}*A*, where *R* is the radius of the sphere and *A* is the angle of the lune in radians.

Three great circles that do not intersect in a single pair of antipodal points form eight spherical triangles on the sphere (Figure 1,4). If the elements, that is, the angles and sides, of one of the triangles are known, the elements of the other triangles can be easily found. For this reason, the relations between the elements of only one triangle are usually considered; the sides of this triangle are minor arcs of the great circles. The measures of the sides *a, b*, and *c* of a spherical triangle are equal to the measures of the corresponding plane angles of the trihedral angle *OABC* (Figure 1,5); the measures of the angles *A, B*, and *C* of the triangle are equal to the measures of the corresponding dihedral angles of the trihedral angle.

Spherical triangles differ in several respects from triangles in the plane. For example, in the case of spherical triangles, the three necessary and sufficient conditions for the congruence of plane triangles are supplemented by a fourth necessary and sufficient condition: two triangles are congruent if their corresponding angles are equal (there are no similar triangles on a sphere).

Congruent spherical triangles are spherical triangles that can be made to coincide by means of motions on the sphere. It therefore follows that congruent spherical triangles have equal elements and the same orientation. Triangles with equal elements and different orientation are said to be symmetric—for example, the triangles *AC’C* and *BCC’* in Figure 1,6.

In any spherical triangle formed by minor arcs of great circles, the sum of any two sides is greater than the third side, and the difference between any two sides is less than the third side. The sum of the sides is always less than 2π. The sum of the angles of a spherical triangle is always less than 3π and greater than π. The difference *s* – π = ∊, where *s* is the sum of the angles of a spherical triangle, is called the spherical excess. The area of a spherical triangle is given by the formula *S* = *R*^{2}∊, where *R* is the radius of the sphere.

The position of any point on the sphere is completely determined by specifying two numbers. A description follows of a way by which these numbers, or coordinates, may be defined (Figure 1,7).

Some great circle *QQ’* is taken as the equator. One of the two points, say *P*, where the diameter *PP’* of the sphere perpendicular to the plane of the equator intersects the surface of the sphere, is taken as the pole. Finally, a great semicircle *PAP’* emanating from the pole is taken as the zero meridian. The great semicircles of a sphere emanating from *P* are called meridians, and the small circles parallel to the equator are called parallels. The angle θ = *POM*, called the polar distance, is taken as one of the coordinates of a point *M* on the sphere, and the angular distance ɸ = *AON* between the zero meridian and the meridian through *M* is taken as the other coordinate, which is called the longitude and is reckoned counterclockwise.

The use of coordinates on the sphere permits spherical figures to be studied by means of the methods of analytic geometry. For example, the two equations

θ= *f(t)* ɸ = *g(t)*

or the single equation

*F*(θ, ɸ) = 0

involving the coordinates θ and ɸ define a curve on the sphere. The length L of an arc *M*_{1}*M*_{2} of the curve is calculated by means of the formula

where *t*_{1} and *t*_{2} are values of the parameter *t* at the end points *M*_{1} and *M*_{2} of *M*_{1}*M*_{2} (Figure 1,8).

### REFERENCES

Stepanov, N. N.*Sfericheskaia trigonometriia*, 2nd ed. Leningrad-Moscow, 1948.

*Entsiklopediia elementarnoi matematiki*, book 4:

*Geometriia*. Moscow, 1963.