ALBERT

Description: In this work we present the observational study of propagation of blobs (Sheeley et al., 1997) in which detection in the white-light data is favored during solar minimum activity. Therefore, the minimum of the solar cycle 24 was particularly an optimal occasion to perform an observational analysis of the detection of blobs. As blobs are considered to be tracers in white-light data of the slow solar wind, the importance of the study of their propagation has two aims: (1) to known more about their kinematic behavior and (2) to inquire about the local morphology of the solar magnetic field of their origin. The selected periods of observation have permitted the identification of around 100 blob-like structures detected by LASCO and SECCHI coronagraphs on board SOHO and STEREO, respectively. The inferring location of their origin in the inner solar corona was performed by the tridimensional Potential Field Source Surface (PFSS) developed by De Rosa (2003). The results of this study support previous findings that track down the origin of the slow and intermediate solar wind to neighboring regions of helmet streamers and pseudostreamers (Panasenco and Velli, 2016; Riley and Luhmann, 2012, and references therein). In addition, the kinematic of the 3D trajectories of blobs have been used to explore the 'drag-force' model (Borgazzi et al., 2009) which explains the stretching behavior of faster and slower blobs. Finally in this study, we propose a "new" estimation of the Sun-mass-loss taking into account also the blobs mass along an 11-years solar cycle.

Description: The two main types of coronal streamers, pseudostreamers and helmet streamers, have different magnetic topologies. However, these coronal streamers present one or more cavities which can become unstable and result in filament eruptions and coronal mass ejections. In this study, we evaluate the physical and magnetic properties of pseudostreamers and helmet streamers using magnetograms, EUV and white light data, and potential-field and non-linear force-free field (NLFFF) models. We compare the observed pseudostreamer cavities with helmet-streamer cavities to evaluate similarities and differences. We also study the relation between magnetic and physical properties and (in)stability. Understanding the physical and magnetic characteristics of coronal-streamer cavities can provide key information on the evolution of these large coronal structures. This work is supported by NASA grant 80NSSC20K1445 to the Smithsonian Astrophysical Observatory.