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1927 G. D. Birkhoff Relativity & Mod. Physics (ed. 2) xv. 255 The most general solution can be obtained from the Schwarzschild solution by a proper choice of coördinates.

1934 R. C. Tolman Relativity, Thermodynamics, & Cosmol. 208 There are..three consequences which can be obtained from the Schwarzschild line element which can be used to distinguish between the relativistic and Newtonian theories of gravitation.

1939 Ann. Math. 40 924 In the case of a Schwarzschild field a particle is bound to follow a path with a radius greater than (2 + √3) times the radius of the Schwarzschild singularity.

1957 Physical Rev. 108 1067/2 This transformation is not acceptable..because it assumes Euclidean rather than Schwarzschild geometry for the displacement.

1957 Physical Rev. 108 1067/2 We get the difference between the Schwarzschild metrics for the two reduced masses.

1957 Physical Rev. 108 1068/2 The effective potential starts from 0 at the Schwarzschild radius, rises to a maximum and then falls off again to zero at very large r.

1965 B. K. Harrison et al. Gravitation Theory & Gravitational Collapse 157 Introduce Schwarzschild coordinates ds² = [etc.]..as well as the baryon number coordinate.

1966 R. Akerib tr. M. A. Tonnelat Einstein's Unified Field Theory v. 82 This is the Schwarzschild solution of the field equations. It defines completely the gravitational field in the neighborhood of attractive masses and permits the determination of the trajectories of particles moving in it.

1968 Robertson & Noonan Relativity & Cosmology ix. 236 The Schwarzschild line element has at the radius 2μ a singularity known as the Schwarzschild singularity.

1968 Sears & Brehme Introd. Theory of Relativity xi. 200 If the Schwarzschild singularity did exist, the Schwarzschild radius would be the radius of a spherical surface which separates the universe into two parts which are isolated from one another by the fact that local time does not elapse at the bounding surface.

1968 Commun. Math. Physics VIII. 245 In the special case where the gravitational coupling of the electromagnetic energy density is neglected..all solutions are computed explicitly, thus extending an earlier result of Ginzburg for a magnetic dipole in Schwarzschild's space-time.

1969 Nature 16 Aug. 690/1 Nothing can ever pass outwards through the Schwarzschild sphere of radius r = 2GM/c².

1970 Nature 4 Apr. 64/2 The metric used to describe the geometry of space-time in the vicinity of the collapsed object in this and other papers..has been the spherically symmetric Schwarzschild metric, which is valid only if the collapsed object has zero angular momentum.

1971 Jrnl. Math. Physics 12 1846/1 We consider the problem of a point charge slowly lowered into a Schwarzschild black hole as a simple example where the final outcome can be investigated.

1973 C. W. Misner et al. Gravitation xxiii. 597 The above discussion identifies the Schwarzschild coordinates..by their intrinsic geometric properties. Not only are r and t radial and time variables, respectively (in that ∂/∂r and ∂/∂t are spacelike and timelike, respectively..), but they have particular properties..that distinguish them from other possible coordinate choices... No claim is made that they are the only coordinates that might reasonably be called r and t.

1973 Physics Bull. Nov. 654/3 An observer falling with the surface of the collapsing star has his light cones squashed as he reaches the Schwarzschild surface of radius 2GM/c²; he finds it ever more difficult to signal to distant observers as collapse proceeds. He will appear to them to fall ever more slowly as he approaches the critical surface, and never actually reach it.

1974 Nature 5 July 17/1 In essence the significance of the Schwarzschild surface at r = R_s must have been known to Eddington, certainly by the early 1930s.

1974 Nature 5 July 17/1 Once inside the Schwarzschild sphere, one cannot communicate with the world outside; and moreover, one would inexorably be propelled towards the centre: not all the King's horses nor all the King's men can prevent it from happening.

1974 Nature 5 July 37/2 There is no creation of massless particles in the exterior region of a Schwarzschild black hole, which is the static end state reached as a result of spherically symmetric gravitational collapse.

1974 Encycl. Brit. Macropædia XV. 587/1 The most conspicuous feature of the Schwarzschild field is that if the total mass is thought of as concentrated at the very centre, then at a finite distance from that centre, the Schwarzschild radius, the geometry of space-time changes drastically from that to which we are accustomed.

1977 Sci. Amer. Jan. 34/3 For a star of about 10 solar masses the Schwarzschild radius is about 30 kilometres.