The sun is a plasma threaded variously by magnetic fields that stretch from the deep interior to the heliosphere. These fields can couple various layers together and transfer momentum between different parts of the solar interior. The sun is not a rigid body and there is no requirement from conservation of angular momentum that the overall solar rotation rate as measured at the photosphere need remain constant. At the 150-foot solar tower telescope on Mt. Wilson the Doppler shift, magnetic fields and line intensity of the solar photosphere have been measured as often as possible beginning in 1965 (1965 and 1966 were lost in a data handling mistake). The overall rotation rate is determined for each observation by fitting the observed photospheric velocities to the function ωsid(φ) =A+Bsin2(φ) +Csin4(φ) where φ is latitude, to determine what is known as the A coefficient. We are currently re-reducing all the data from the 150-foot tower system. Differential rotation is described by the B and C coefficients which we are holding constant with average values. The velocities come from Doppler shifts which with a Babcock magnetograph come mostly from the displacement of the moving sampling stage which balances the intensity in the wings of the spectral line. Line shape calibration uncertainties do not influence this shift. We find variations in the global rotation rate which are larger than the shifts known as the torsional oscillations. If the B and C coefficients are fitted to each Dopplergram the torsional oscillations become evident. Instrument changes of the exit slit system and spectrograph grating do not introduce jumps in the A coefficient. Restriction of observations to those when the sun is within 40 degrees of local noon leaves the result essentially unchanged. There may be a solar cycle influence but, the resulting pattern shown in the attached figure is more complex than that. Data from before 1983 has a scatter about 3 times larger than what is shown here with an average consistent with these results. However, the larger scatter prevents the variability from being evident.

5 For the first time, we simulate the detailed spectral line emission from a solar active 6 region (AR) with the Alfvén Wave Solar Model (AWSoM). We select an AR appearing 7 near disk center on 2018 July 13 and use an NSO/HMI synoptic magnetogram to specify 8 the magnetic field at the model’s inner boundary. To resolve smaller-scale magnetic 9 features, we apply adaptive mesh refinement to resolve the AR with a horizontal spatial 10 resolution of 0.35 • (4.5 Mm), four times higher than the background corona. We then 11 apply the SPECTRUM code informed with CHIANTI spectral emissivities to calculate 12 spectral lines forming at temperatures ranging from 0.5 to 3 MK. Comparisons are 13 made between the simulated line intensities and those observed by the Hinode/EIS 14 instrument where we find close agreement (about 20% relative error for both loop top 15 and footpoints at a temperature of about 1.5 MK) across a wide range of loop sizes and 16 temperatures. We also simulate and compare Doppler velocities and find that simulated 17 flow patterns are of comparable magnitude to what is observed. Our results demonstrate 18 the broad applicability of the low-frequency Alfvén wave balanced turbulence theory 19 for explaining the heating of coronal loops. 20