Berlin Notebook Gravitational Lens Calculation
During work recorded in a 1912 notebook, Einstein calculated how a foreground mass could bend light from a background source and produce the geometry of a gravitational lens.
Albert Einstein ยท Place
123 Einstein records associated with Berlin.

During work recorded in a 1912 notebook, Einstein calculated how a foreground mass could bend light from a background source and produce the geometry of a gravitational lens.
Einstein's notebook analysis showed that gravitational deflection could allow light from one distant source to reach an observer along two paths, producing two apparent images.
Einstein worked out a magnification relation for the gravitational-lens configuration, anticipating formulae he would publish when he returned to the subject decades later.
Moves to Berlin for a senior research appointment and membership of the Prussian Academy of Sciences.
Publishes work refining the mathematical and covariance problems of his developing gravitational theory.
Einstein defended the restricted covariance of his provisional gravitational equations, believing at the time that broader coordinate freedom would prevent a unique physical description.
Continues with Grossmann to examine covariance properties of their gravitational equations, exposing problems that eventually drive Einstein back toward general covariance.
Einstein gave a systematic mathematical presentation of the Entwurf gravitational theory after moving to Berlin, clarifying its field equations, coordinate restrictions and physical assumptions.
Publishes a detailed formal treatment of the developing gravitational theory, presenting its mathematical structure before he restores fully general covariance.
Einstein investigated how energy and momentum conservation should be formulated when the gravitational field itself participates in the dynamics of spacetime.
Co-signs a pacifist appeal opposing wartime nationalism among European intellectuals.
With Adriaan Fokker, reformulates Nordstrom's competing gravitation theory using tensor methods, clarifying how relativistic gravity could be expressed geometrically.
Einstein examined rotating coordinate systems as a demanding consistency test for the Entwurf equations, exposing difficulties that contributed to his later rejection of the provisional theory.
Publishes experimental work with Wander de Haas linking magnetism to angular momentum.
Einstein abandoned key restrictions of the Entwurf approach and returned to generally covariant tensor equations, beginning the final rapid reconstruction of his gravitational theory.
With the completed geometric treatment of gravity, Einstein obtained a solar light-deflection prediction approximately twice the value produced by his earlier equivalence-principle calculation.
Using the completed theory, obtains the full gravitational deflection predicted for starlight grazing the Sun, approximately twice his earlier 1911 estimate.
Einstein presented new gravitational field equations to the Prussian Academy that restored much broader covariance and marked the first of his decisive November 1915 communications.
Presents revised gravitational field equations to the Prussian Academy during his final push toward general relativity.
Einstein refined his field equations under a trace condition and showed how the revised framework could approach fully covariant gravitation in regions outside matter.
Presents improved gravitational equations to the Prussian Academy and moves substantially closer to the generally covariant form completed later that month.
Presents another formulation of gravitation using a restricted coordinate condition with unit determinant.
The relativistic Mercury calculation matched the anomalous perihelion advance using the gravitational theory itself rather than introducing an additional planet or an adjustable correction to Newtonian gravity.
Explains Mercury's anomalous perihelion advance using the emerging general theory of relativity.
Einstein used the emerging general theory to account for Mercury's unexplained perihelion advance, obtaining the observed residual shift that earlier gravitational models had failed to reproduce.
Presents the final generally covariant gravitational field equations to the Prussian Academy, completing the mathematical core of general relativity.
Presents the final generally covariant gravitational field equations to the Prussian Academy.
Einstein presented the final generally covariant field equations including their coupling to matter, completing the mathematical core of general relativity.
Einstein mentioned the possibility of gravitational lensing in a letter to Heinrich Zangger, revisiting the double-image effect he had calculated in his 1912 notebook.
Einstein represented the probability of an atom absorbing incident radiation and moving to a higher energy state with a coefficient proportional to the surrounding radiation density.
Einstein formulated radiation processes in terms of probabilities for transitions between atomic energy states, creating a statistical framework for absorption and emission.
Einstein required upward and downward atomic transitions to balance in thermal equilibrium, using that condition to connect transition probabilities with the equilibrium radiation spectrum.
Develops the treatment of energy and momentum in the gravitational field, addressing how conservation laws operate within the generally covariant theory.
Publishes a systematic presentation of the general theory of relativity and its field equations.
Einstein published a comprehensive exposition of general relativity that assembled the geometric framework, field equations and physical consequences into a systematic theory.
Einstein's mature theory described freely falling bodies as following the straightest possible world-lines through curved spacetime rather than being pulled by a Newtonian gravitational force.
Serves as president of the German Physical Society during the consolidation of general relativity.
Einstein developed a gravitational energy-momentum construction to discuss how changing gravitational fields can transport energy despite the special conservation difficulties of general relativity.
Einstein's wave analysis showed that physical gravitational disturbances in the relativistic theory propagate through empty space at the speed of light.
Formulates general relativity using Hamilton's variational principle, providing a compact mathematical route to the gravitational field equations and their conservation properties.
Responds to Friedrich Kottler's criticism of the equivalence hypothesis, defending the conceptual basis on which his route from special to general relativity depended.
Einstein's field equations made gravity nonlinear, so the gravitational field contributes to the dynamics instead of behaving as a simple superposition of independent Newtonian forces.
Einstein showed that his statistical rules for absorption, spontaneous emission and induced emission can reproduce Planck's black-body radiation law under thermal equilibrium.
Develops a quantum theory of radiation introducing transition probabilities later represented by Einstein coefficients.
Einstein treated the frequency of absorbed or emitted radiation as fixed by the discrete energy difference between the participating atomic states.
Einstein introduced a coefficient describing the probability that an excited atom will emit radiation spontaneously and fall to a lower energy state.
Einstein introduced a second radiation-dependent transition probability in which incident radiation stimulates an excited atom to emit additional radiation.
General relativity connected spacetime curvature with the energy, momentum and stresses of matter, making the physical contents of the universe sources of the gravitational geometry.
Einstein linearised the gravitational field equations in the weak-field limit and identified wave-like disturbances capable of propagating through spacetime.
Communicates Karl Schwarzschild's exact solution of the new field equations to the Prussian Academy, demonstrating that general relativity admits important exact solutions.
Predicts gravitational waves as propagating disturbances in spacetime within general relativity.
Publishes his popular introduction to special and general relativity.
By assigning momentum to individual radiation quanta, Einstein concluded that atoms must recoil when they emit or absorb directed packets of light.
To support a static cosmological solution, Einstein modified the gravitational field equations with an additional cosmological term that could counterbalance large-scale attraction.
Becomes founding director of the Kaiser Wilhelm Institute for Physics.
Einstein's radiation theory assigned each emitted or absorbed light quantum a momentum equal to its energy divided by the speed of light.
Einstein designed his early relativistic cosmology partly around the hope that inertia would be determined by the overall distribution of matter, reflecting his interpretation of Mach's ideas.
Einstein united discrete atomic transitions with thermodynamic equilibrium, demonstrating that quantum absorption and emission rules could generate the observed black-body spectrum.
Einstein showed that randomly directed quantum emission events contribute to molecular momentum fluctuations and must be balanced statistically in thermal equilibrium.
Applies general relativity to the universe and introduces the cosmological constant in a static cosmological model.
Einstein's published quantum theory of radiation formalized spontaneous emission as an intrinsically statistical process occurring without an externally applied radiation field.
Einstein applied general relativity to the universe as a whole and proposed a spatially closed, homogeneous model intended to remain static on cosmic scales.
Formulates stimulated emission in his quantum theory of radiation, a principle later fundamental to lasers.
Einstein's equilibrium analysis required an induced emission process in which incident radiation increases the probability that an excited atom emits matching radiation.
Einstein revisited his gravitational-wave analysis and corrected the treatment of radiated energy, removing misleading wave modes from the earlier calculation.
Publishes a foundational discussion of general relativity in which he explicitly names Mach's principle and distinguishes it from the equivalence and relativity principles.
Einstein showed that the leading gravitational radiation from an isolated slow-moving system is governed by changes in its mass quadrupole moment rather than by a simple mass dipole.
Refines gravitational-wave theory and derives the quadrupole form for radiated energy.
Derives the quadrupole formula for gravitational radiation, relating emitted wave power to changing mass distributions in accelerating systems.
Becomes internationally famous after eclipse observations are widely reported as confirming general relativity.
Publicly confronts organized attacks on relativity amid growing political and antisemitic hostility.
Publishes a proposed addition to the foundations of general relativity, continuing his effort to strengthen the conceptual and mathematical basis of gravitational field theory.
Awarded the 1921 Nobel Prize in Physics for theoretical physics, especially the law of the photoelectric effect.
Explains how geometry acquires physical meaning through measurement and discusses the relationship between mathematical geometry and the spacetime structure of general relativity.
Begins sustained attempts to combine gravitation and electromagnetism within a single field framework.
The Nobel citation singled out Einstein's quantitative law of the photoelectric effect, giving formal recognition to a result rooted in his 1905 light-quantum hypothesis.
The Royal Swedish Academy of Sciences announced Einstein as the recipient of the reserved 1921 Nobel Prize in Physics, emphasizing his discovery of the law of the photoelectric effect.
Explores an affine field theory as a possible extension of general relativity, seeking a unified geometric description of gravitation and electromagnetism.
The emerging evidence from Compton scattering gave strong experimental support to the energy-and-momentum properties of radiation quanta that Einstein had advocated for years.
Publishes a further Prussian Academy paper on general relativity, revisiting technical aspects of the theory after its rapid international acceptance.
Experimental scattering results increasingly supported the view that individual radiation quanta carry directed momentum, a requirement already embedded in Einstein's 1917 radiation theory.
Is admitted to the Pour le Mรฉrite for Sciences and Arts.
Einstein recognized that Bose's counting method obtained Planck's spectrum by treating light quanta statistically without relying on the classical independent-particle counting used for ordinary gases.
Satyendra Nath Bose sent Einstein a manuscript deriving Planck's radiation law by a new statistical counting method applied directly to indistinguishable light quanta.
Translates Satyendra Nath Bose's paper on Planck's law into German and arranges its publication.
Predicts that ideal bosonic particles can accumulate in the lowest quantum state at low temperature.
Extends Bose's statistical method from photons to particles of an ideal gas.
Einstein submitted Bose's translated paper for publication and endorsed its new derivation of the black-body radiation law from quantum statistics.
Einstein translated Bose's manuscript on the quantum statistics of radiation into German after recognizing the importance of its treatment of light quanta.
Bose's method, promoted by Einstein, treated light quanta as statistically indistinguishable objects, an idea that became fundamental to quantum statistics.
Accepts election as a Foreign Honorary Member of the American Academy of Arts and Sciences.
Einstein continued to favour exact energy and momentum conservation in individual radiation processes rather than the merely statistical conservation proposed by the Bohr-Kramers-Slater approach.
Einstein drew an analogy between the wave-particle duality he had identified for radiation and the emerging wave description of material particles, reinforcing the broader quantum duality concept.
Joins the administrative council of the Hebrew University of Jerusalem.
Engages critically with the emerging matrix and wave formulations of quantum mechanics.
Publishes further work on the quantum theory of the ideal monatomic gas.
Publishes a unified field theory of gravitation and electricity, beginning a long programme to extend relativity into a single classical field framework.
Einstein proposed experiments on light emitted by moving canal-ray atoms to test how quantum emission events could coexist with the coherence properties expected from wave optics.
Works with Leo Szilard on safer refrigerator designs without moving mechanical parts.
Reconsiders Theodor Kaluza's five-dimensional approach after developments by Oskar Klein, seeing new possibilities for unifying gravitation and electromagnetism geometrically.
Emil Rupp reported experimental results that appeared to support Einstein's proposed coherence tests, although the measurements were later recognized as unreliable and fraudulent.
Collaborates with Emil Rupp on proposed tests of whether atomic radiation behaves as waves or quanta.
Studies and discusses Schrรถdinger's wave mechanics while questioning its physical interpretation.
Einstein devised a wire-grid arrangement intended to probe the coherence length and wave character of radiation emitted in individual atomic processes.
With Jakob Grommer, investigates whether the motion of particles can be derived from the gravitational field equations rather than imposed as a separate law.
Investigates with Jakob Grommer whether particle motion can follow directly from gravitational field equations.
Presents Academy papers on Kaluza's connection between gravitation and electricity, deriving important aspects of the five-dimensional unified-field framework.
Introduces a geometry that preserves distant parallelism, adopting teleparallel structures as a new mathematical basis for attempts to unify gravity and electromagnetism.
Patent work with Leo Szilard advances an absorption refrigerator using electromagnetic pumping concepts.
Develops the teleparallel unified-field programme, replacing ordinary Riemannian geometry with tetrad-based structures intended to encompass gravitation and electromagnetism together.
Develops a unified-field approach using distant parallelism, also called teleparallel geometry.
Einstein adopted tetrad fields and distant parallelism as a new geometric language in an attempt to place gravitation and electromagnetism inside one unified classical field theory.
Employs Helen Dukas as his secretary and assistant, beginning a long professional association.
Publishes a unified field formulation based on distant parallelism and Hamilton's principle, continuing his search for equations joining gravitational and electromagnetic fields.
Publishes a widely publicized unified-field theory based on teleparallel geometry.
Receives the inaugural Max Planck Medal for outstanding achievement in theoretical physics.
Lectures at Harnack House on the problem of space and ether, revisiting how relativity changes the physical interpretation of spacetime and field structure.
Publishes work with Walther Mayer giving exact static solutions of unified-field equations, testing whether the programme can represent physically meaningful configurations.
Further develops spaces combining a Riemann metric with distant parallelism, refining the geometric machinery behind his teleparallel unified-field theory.
Examines the compatibility of equations in the unified-field programme, addressing mathematical consistency before the theory can be regarded as physically viable.
Adopts an expanding cosmological model and abandons the need for his earlier static-universe construction.
Publishes a non-static cosmological model within general relativity, accepting cosmic expansion and dispensing with the static balance that motivated his cosmological constant.
Publishes another unified theory of gravitation and electricity, continuing to test alternative geometrical structures beyond the standard equations of general relativity.