Constraints on Physical Models of Solar Variability From Stellar Observations

Details Constraints on Physical Models of Solar Variability From Stellar Observations Constraints on Physical Models of Solar Variability From Stellar Observations

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp32b02r&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SP32B-02 INVITED

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7537 Solar And Stellar Variability

Scientific paper

Stars with the same temperature, luminosity, chemical composition, and average activity level as the Sun may properly be termed "sunlike" stars. The variability of several dozen more-or-less sunlike stars has been monitored regularly in chromospheric Ca II HK emission for 35 years, and photometrically for over 15 years. A qualitative comparison of solar variability with its stellar analogs indicates that the Sun's current behavior is not unusual among sunlike stars. We know that the amplitude of the year-to-year photometric variation for young, active stars is typically several percent, and that it decreases dramatically among stars more closely resembling the Sun in age and average activity to a level approaching the solar value of about 0.1%. Some observations do, however, suggest that the amplitude of the Sun's cyclic variation, measured photometrically, may be somewhat small relative to that of other sunlike stars. The stellar measurements imply that a true luminosity change underlies the cyclic irradiance variation of the Sun and other sunlike stars. The amplitude discrepancy may be due in part to an irradiance effect arising from viewing geometry. Overall, the standard model of solar variability invoking spots, faculae, and active regions can explain the stellar observations reasonably well without doing violence to either.

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