Chronology of Stellar Astronomy

-134 Hipparchus creates the magnitude scale of stellar apparent luminosities.
1596 David Fabricus notices that Mira's brightness varies.
1672 Geminiano Montanari notices that Algol's brightness varies.
1686 Gottfried Kirch notices that Chi Cygni's brightness varies.
1718 Edmund Halley discovers stellar proper motions by comparing his astrometric measurements with those of the Greeks.
1782 John Goodricke notices that the brightness variations of Algol are periodic and proposes that it is partially eclipsed by a body moving around it.
1784 Edward Piggot discovers the first Cepheid variable star.
1838 Thomas Henderson, Friedrich Struve, and Friedrich Bessel measure stellar parallaxes.
1844 Friedrich Bessel explains the wobbling motions of Sirius and Procyon by suggesting that these stars have dark companions.
1906 Arthur Eddington begins his statistical study of stellar motions.
1908 Henrietta Leavitt discovers the Cepheid period-luminosity relation.
1910 Ejnar Hertzsprung and Henry Russell study the relation between magnitudes and spectral types of stars.
1924 Arthur Eddington develops the main-sequence mass-luminosity relationship.
1929 George Gamow proposes hydrogen fusion as the energy source for stars.
1938 Hans Bethe and Carl von Weizsacker detail the proton-proton chain and CNO cycle in stars.
1939 Rupert Wildt realizes the importance of the negative hydrogen ion for stellar opacity.
1952 Walter Baade distinguishes between Cepheid I and Cepheid II variable stars.
1953 Fred Hoyle predicts a carbon-12 resonance to allow stellar triple alpha reactions at reasonable stellar interior temperatures.
1961 Chushiro Hayashi publishes his work on the Hayashi track of fully convective stars.
1963 Fred Hoyle and William Fowler conceive the idea of supermassive stars.
1964 Subrahmanyan Chandrasekhar and Richard Feynman develop a general relativistic theory of stellar pulsations and show that supermassive stars are subject to a general relativistic instability.
1967 Gerry Neugebauer and Eric Becklin discover the Becklin-Neugebauer object at 10 microns.