The Introduction of Absolute Magnitude (1902 - 1922)

Details The Introduction of Absolute Magnitude (1902 - 1922) The Introduction of Absolute Magnitude (1902 - 1922)

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006jahh....9..173h&link_type=abstract

Journal of Astronomical History and Heritage (ISSN 1440-2807), Vol. 9, No. 2, p. 173 - 179 (2006).

Astronomy and Astrophysics

Astronomy

Stellar Luminosity, Parallax, Absolute Magnitude, H-R Diagram

Scientific paper

The absolute magnitude of a star, this being the apparent magnitude that a star would have if it was moved to a distance of 10 parsecs from the observer, is a ubiquitous concept and is commonly used by today's astronomers to represent the luminosity of a star. This short paper traces the history of the expression 'absolute magnitude' from the time of its introduction in 1902 by its originator J.C. Kapteyn, up to the ratification of its acceptance by the International Astronomical Union at its first meeting in 1922.

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