| 释义 |
Schwarzschild|ˈʃvɑːtsʃiːlt, ˈʃwɔːtstʃaɪld|
The name of Karl Schwarzschild (1873–1916), German astronomer, used attrib. and in the possessive to designate various concepts developed by him or arising from his work.
1. Photogr. Used with reference to a quantitative law of reciprocity failure in emulsions.
1920Jrnl. Optical Soc. Amer. IV. 272 If Schwarzschild's law is correct, the reciprocity law does not hold for any value of the intensity, the error being the same in percentage amount for all intensities. 1942C. E. K. Mees Theory of Photographic Process vi. 236 Schwarzschild (1899) confirmed Abney's results that the reciprocity law is not valid and concluded that a constant effect is produced so long as the condition Itp = constant is satisfied, in which p is constant and equal to about 0.8. This relation, with p constant, came to be generally known as Schwarzschild's law and is frequently referred to by this name today. 1960G. E. Lockie tr. K. S. Lyalikov's Chem. of Photographic Mechanisms i. i. 58 The Schwarzschild equation is not valid for the range of exposures used in this investigation.
2. Physics. Denoting concepts arising out of the exact solution of Einstein's field equations described by Schwarzschild soon after the publication of the general theory of relativity (Sitzungsber. der k. preuss. Akad. der Wissensch. (1916) 189, 424), as Schwarzschild coordinate, Schwarzschild field, Schwarzschild geometry, Schwarzschild horizon, Schwarzschild solution, Schwarzschild space-time, Schwarzschild surface; Schwarzschild black hole, a static, non-rotating, and uncharged black hole, i.e., an object postulated to result from the complete gravitational collapse of an electrically neutral and non-rotating body, and which has a physical singularity at the centre of its Schwarzschild sphere to which the infalling matter inevitably proceeds and at which the curvature of space-time is infinite; Schwarzschild line element, (a) a scalar representation of the Schwarzschild metric, being an expression for the separation of two adjacent points in the space-time of Schwarzschild geometry; (b) loosely = Schwarzschild metric (a); Schwarzschild metric, (a) a mathematical description of the geometry of space-time exterior to a non-rotating body, usu. expressed as a tensor in differential geometry; (b) loosely = Schwarzschild line element (a); Schwarzschild radius, the radius of the Schwarzschild sphere; Schwarzschild singularity, a singularity in coordinates, but not a physical singularity in space-time, occurring at the Schwarzschild radius; Schwarzschild sphere, the effective boundary or horizon of a Schwarzschild black hole, which infalling matter reaches in an infinite time as seen by an external observer but a finite time in the reference frame of the matter, and at which the escape velocity is infinite, so that the escape of matter or radiation from the inside is impossible except by a postulated quantum-mechanical process.
1927G. 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. 1934R. C. Tolman Relativity, Thermodynamics & Cosmology 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. 1939Ann. Math. XL. 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. 1957Physical Rev. CVIII. 1067/2 This transformation is not acceptable..because it assumes Euclidean rather than Schwarzschild geometry for the displacement. Ibid., We get the difference between the Schwarzschild metrics for the two reduced masses. Ibid. 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. 1965B. K. Harrison et al. Gravitation Theory & Gravitational Collapse 157 Introduce Schwarzschild coordinates ds2 = [etc.]..as well as the baryon number coordinate. 1966R. Akerib tr. M. A. Tonnelat's 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. 1968Robertson & Noonan Relativity & Cosmology ix. 236 The Schwarzschild line element has at the radius 2µ a singularity known as the Schwarzschild singularity. 1968Sears & 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. 1968Commun. Math. Physics VIII. 245 In the special case where the gravitational coupling of the electromagnetic energy density is neglected..all solutions are computed explicity, thus extending an earlier result of Ginzburg for a magnetic dipole in Schwarzschild's space-time. 1969Nature 16 Aug. 690/1 Nothing can ever pass outwards through the Schwarzschild sphere of radius r = 2GM/c2. 1970Ibid. 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. 1971Jrnl. Math. Physics XII. 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. 1973C. 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. 1973Physics 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. 1974Nature 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. Ibid. 17/1 In essence the significance of the Schwarzschild surface at r = Rs must have been known to Eddington, certainly by the early 1930s. Ibid., 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. 1974Encycl. 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. 1977Sci. Amer. Jan. 34/3 For a star of about 10 solar masses the Schwarzschild radius is about 30 kilometres. |