Authors: Cynthia López-Portela (NASA-UMBC), Nicholeen Viall (NASA), Samantha Wallace (Embry-Riddle Aeronautical University)

Mesoscale density structures form part of the solar wind and a subset of them are named ‘blobs’. Using the multipoint white-light observations of LASCO/SOHO and SECCHI/STEREO, we perform the calculation of the deprojected components of blobs along their radial (elongation) and transverse (width) direction, in order to study their morphological evolution along these two directions as they flow outwardly from the Sun. In solar minima, the magnetic structure that typically forms and allocates at equatorial latitudes on the Sun, are helmet streamers (HSs), formed by coronal holes (CHs) with opposite polarities. As the solar activity increases, the coronal magnetic field becomes more complex and additionally to HSs, unipolar streamers are formed and known as pseudostreamers (PSs). In white-light images, these different magnetic structures can all be along the same line-of-sight (LOS), challenging the identification of which topology produced different types of blobs. Therefore, to be able to localize with high precision the type of magnetic structures that give birth to our sample of blobs, we implement the ADAPT-WSA model to relate the 3D-coordinates of blobs to their S-web origin, during solar minima of solar cycle 23, and the ascending and descending phases of solar cycle 24.