Modelling solar irradiance from ground-based photometric observations

Theodosios Chatzistergos,Fabrizio Giorgi,Ilaria Ermolli,Cosmin Constantin Puiu,Natalie A Krivova

doi:10.1051/swsc/2020047

Abstract

Total solar irradiance (TSI) has been monitored from space since 1978, i.e. for about four solar cycles. The measurements show a prominent variability in phase with the solar cycle, as well as fluctuations on timescales shorter than a few days. However, the measurements were done by multiple and usually relatively short-lived missions. The different absolute calibrations of the individual instruments and the unaccounted for instrumental trends make estimates of the possible long-term trend in the TSI highly uncertain. Furthermore, both the variability and the uncertainty are strongly wavelength-dependent. While the variability in the UV irradiance is clearly in-phase with the solar cycle, the phase of the variability in the visible range has been debated. In this paper, we aim at getting an insight into the long-term trend of TSI since 1996 and the phase of the solar irradiance variations in the visible part of the spectrum. We use independent ground-based full-disc photometric observations in Ca II K and continuum from the Rome and San Fernando observatories to compute the TSI since 1996. We follow the empirical San Fernando approach based on the photometric sum index. We find a weak declining trend in the TSI of $ {-7.8}_{-0.8}^{+4.9}\times 1{0}^{-3}$ Wm−2 y−1 between the 1996 and 2008 activity minima, while between 2008 and 2019 the reconstructed TSI shows no trend to a marginally decreasing (but statistically insignificant) trend of $ {-0.1}_{-0.02}^{+0.25}\times 1{0}^{-3}$ Wm−2 y−1. The reference TSI series used for the reconstruction does not significantly affect the determined trend. The variation in the blue continuum (409.2 nm) is rather flat, while the variation in the red continuum (607.1 nm) is marginally in anti-phase, although this result is extremely sensitive to the accurate assessment of the quiet Sun level in the images. These results provide further insights into the long-term variation of the TSI. The amplitude of the variations in the visible is below the uncertainties of the processing, which prevents an assessment of the phase of the variations.

Highlights

The solar irradiance (SI) is an important parameter in studies of the solar variability and Earth’s climate
Results from the various SI models show considerable disagreement in the long-term evolution of Total solar irradiance (TSI) with estimated changes since the Maunder minimum ranging from 0.7 WmÀ2 to 6 WmÀ2 (Wang et al, 2005; Krivova et al, 2007, 2010; Tapping et al, 2007; Steinhilber et al, 2009; Shapiro et al, 2011; Vieira et al, 2011; Judge et al, 2012, 2020; Egorova et al, 2018; Wu et al, 2018; Lockwood & Ball, 2020)
To improve our understanding of the solar-cycle and long-term variability of SI, here we analyse the TSI and spectral solar irradiance (SSI) variations in two spectral intervals in the Vis over the last two solar cycles derived from a careful analysis of two independent series of ground-based solar observations

Summary

Introduction

The solar irradiance (SI) is an important parameter in studies of the solar variability and Earth’s climate. The spectrallyresolved SI, called the spectral solar irradiance (SSI), is defined as the solar radiative energy flux per unit area and wavelength as measured at the top of the Earth’s atmosphere at a mean distance of one astronomical unit. Measurements collected since 1978 by a series of instruments show that the TSI varies at all discernible timescales from. On timescales longer than the solar cycle, TSI changes are rather uncertain due to the uncertainties in instrumental calibrations and the limited duration of the individual space experiments. There are currently four composite records of TSI measurements, presented by Willson (1997), Dewitte et al (2004), Fröhlich (2006), and Dudok de Wit et al (2017), showing partly conflicting secular trends over the last four solar cycle minima

Results

Discussion

Conclusion