First observations of solar disk gamma rays over a full solar cycle

Abstract

The solar disk is among the brightest $\ensuremath{\gamma}$-ray sources in the sky. It is also among the most mysterious. No existing model fully explains the luminosity, spectrum, time variability, and morphology of its emission. We perform the first analysis of solar disk $\ensuremath{\gamma}$-rays over a full 11 year solar cycle, utilizing a powerful new method to differentiate solar signals from astrophysical backgrounds. We produce: (i) a robustly measured spectrum from 100 MeV to 100 GeV, reaching a precision of several percent in the 1--10 GeV range, (ii) new results on the anticorrelation between solar activity and $\ensuremath{\gamma}$-ray emission, (iii) strong constraints on short-timescale variability, ranging from hours to years, and (iv) new detections of the equatorial and polar morphologies of high-energy $\ensuremath{\gamma}$-rays. We find no significant energy dependence in the time variability of solar disk emission, indicating that strong magnetic-field effects close to the solar surface, rather than modulation throughout the heliosphere, must primarily control the flux and morphology of solar disk emission.