Solar oblateness, a fundamental parameter of the Sun, offers insights into the inner rotation profile, matter distribution, and imposes constraints on General Relativity. However, measuring it is challenging due to its minuscule value, with the solar equator-to-pole radius difference being less than 10 milli-arcseconds (mas). Magnetic activity and instrumental effects related to the space environment can impact measurements. The Helioseismic and Magnetic Imager (HMI) on the Solar Dynamics Observatory (SDO) provided precise determinations of solar oblateness from 2010 to 2023. HMI obtained solar shape measurements during spacecraft roll maneuvers, shifting by 11.25 degrees around the spacecraft-sun line. HMI executed several such roll maneuvers between October 2010 and December 2023. Analysis of HMI data seems to reveal a slight anti-correlation between solar oblateness and solar activity. Applying a new correction method, the mean solar equator-to-pole radius difference at 617.3 nm during 2010–2023 was determined to be 8.75 ± 0.49 mas, equivalent to 6.34 ± 0.35 km at one sigma. The objective of this presentation is to showcase the results obtained with the HMI instrument, which conducts observations in the absorption line of Fe I at 6173Å with a 1-arcsecond resolution. Results will be presented for the four linear polarizations of the telescope (filter sequences 10004, 10005, 10006, and 10007) as well as for the two circular polarizations (filter sequences 10008 and 10009). The evolution of the quadrupole C2 (characteristics of the Sun's gravity field that are due to its non-spherical shape) and hexadecapole C4 (higher-order term that takes into account additional deformations in the Sun's mass distribution) coefficients during a solar cycle will also be presented.