Solar X-ray Intensity vs. Magnetic Flux for Solar Cycle 24

We compare the X-Ray intensity of the solar corona and the photospheric magnetic field using Hinode X-Ray Telescope data and Carrington synoptic magnetic field maps from the Global Oscillating Network for solar cycle 24. We find that the X-Ray intensity is not uniform throughout the cycle with periods of increased X-Ray emission in the active region belts along with high latitude extensions of X-Ray intensity. The high latitude extensions are broken up by periods of decreased X-ray emission in the active region belt and corresponding high latitude coronal holes. We find that the X-Ray intensity has brighter high-latitude X-Ray extensions in the southern hemisphere than in the northern hemisphere with the brightest extension associated with the large active region group that emerged in late 2014. We perform a linear regression fit using the bootstrap method and find the average X-Ray intensity has a power law relationship with the average unsigned magnetic field strength. There is a significant amount of X-Ray emission in quiet sun regions with low magnetic field strengths and that the power law index is lower if these points are included in the linear regression. We find the power law index is lower for the Al-mesh filter than the Be-thin filter, possibly due to emission in the quiet sun. We provide FITS files of the XRT Carrington maps used in this study as a data product for the community.