A method of determining possible brightness variations of the Sun in past centuries from observations of solar-type stars

Details A method of determining possible brightness variations of the Sun in past centuries from observations of solar-type stars A method of determining possible brightness variations of the Sun in past centuries from observations of solar-type stars

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...427l.111z&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 427, no. 2, p. L111-L114

Astronomy and Astrophysics

Astrophysics

50

Brightness, Calcium, H Lines, K Lines, Solar Activity, Solar Constant, Solar Magnetic Field, Variations, Astronomical Photometry, Chromosphere, Chronology, Correlation, Nimbus 7 Satellite, Solar Maximum Mission, Stellar Mass

Scientific paper

Observations of the Sun and a number of stars with mass and age close to the Sun show that changes in magnetic activity and brightness are directly correlated over an activity cycle. The ratio of the two correlated changes shows considerable scatter. If we assume that the scatter represents variability of the one solar-type star at different epochs, the aggregate data may represent the range of variation of the Sun over centuries. We illustrate a technique of inferring possible brightness variations of the Sun from a sample of solar-type stars. The observed scatter of the ratio of all 10 solar-type stars in our sample (stars with (B-V) greater than or approximately equal to 0.55 and less than or approximately equal to 1.2 and mean level of chromospheric activity R primeHK less than or approximately equal to -4.75 in the Lockwood et al. 1992 sample) plus the Sun yields a possible increase of 0.2% - 0.6% in solar brightness as magnetic activity has increased from the Maunder Minimum (ca. A.D. 1660-1710) to the decade of the 1980s. The limited sample of solar-type stars will need to be extended in order to improve the range of the estimate provided.

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