28 Years of Sun-as-a-star Extreme Ultraviolet Light Curves from SOHO EIT

TL;DR

This paper presents a 28-year long time series of Sun-as-a-star EUV light curves from SOHO EIT, capturing solar activity and rotation with high fidelity, useful for stellar and solar studies.

Contribution

The authors convert 28 years of SOHO EIT images into long-term Sun-as-a-star EUV light curves, providing a valuable resource for solar and stellar variability research.

Findings

EUV light curves better trace solar activity cycles than optical data.

Successfully recover solar rotation periods in 93% of years from EUV data.

EUV light curves outperform optical in detecting solar rotation periods.

Abstract

The Solar and Heliospheric Observatory (SOHO) Extreme-ultraviolet Imaging Telescope (EIT) has been taking images of the Solar disk and corona in four narrow EUV bandpasses (171\AA, 195\AA, 284\AA, and 304\AA) at a minimum cadence of once per day since early 1996. The time series of fully-calibrated EIT images now spans approximately 28 years, from early 1996 to early 2024, covering solar cycles 23, 24, and the beginning of cycle 25. We convert this extensive EIT image archive into a time series of `Sun-as-a-star' light curves in EIT's four bandpasses, providing a long-term record of solar EUV variability. These Sun-as-a-star light curves, available for download from https://doi.org/10.5281/zenodo.15474179, trace the Sun as if it were a distant point source, viewed from a fixed perspective. We find that our EUV light curves trace the $\sim$ 11-year solar activity cycle and the $\sim$ 27-day rotation period much better than comparable optical observations. In particular, we can accurately recover the solar rotation period from our 284\AA light curve for 26 out of 28 calendar years of EIT observations (93% of the time), compared to only 3 out of 29 calendar years (10% of the time) of the VIRGO total solar irradiance time series, which is dominated by optical light. Our EIT light curves, in conjunction with Sun-as-a-star light curves at optical wavelengths, will be valuable to those interested in inferring the EUV/UV character of stars with long optical light curves but no intensive UV observations, as well as to those interested in long-term records of solar and space weather.