![Integrating observations and measurements from Parker Solar Probe, Solar Orbiter, and other space- and ground-based observatories](/assets/images/20210507_1200_PFSS_B2_Rss2.5_R1.2_PSP_SO_E8.png)
![Integrating observations and measurements from Parker Solar Probe, Solar Orbiter, and other space- and ground-based observatories](/assets/images/20210507_1200_PFSS_B2_Rss2.5_R1.2_PSP_SO_E8.png)
![Exploring Solar Wind Origins and Connecting Plasma Flows from the Parker Solar Probe to 1 au](/assets/images/solar-surface-height.png)
Exploring Solar Wind Origins and Connecting Plasma Flows from the Parker Solar Probe to 1 au — The magnetic field measurements of the FIELDS instrument on the Parker Solar Probe (PSP) have shown intensities, throughout its first solar encounter, that require a very low source surface (SS) height to be reconciled with
![Large-scale Magnetic Funnels in the Solar Corona](/assets/images/magnetic-funnels.png)
Large-scale Magnetic Funnels in the Solar Corona — We describe open coronal magnetic fields with a specific geometry - large-scale coronal magnetic funnels - that are found to play an important role in coronal dynamics. Coronal magnetic funnels can be attributed to three
![Observations of Solar Wind from Earth-directed Coronal Pseudostreamers](/assets/images/observations-of-solar-wind.png)
Observations of Solar Wind from Earth-directed Coronal Pseudostreamers — Low-speed (<450 km s-1) solar wind is widely considered to originate from streamer loops that intermittently release their contents into the heliosphere, in contrast to high-speed wind, which has its source in large coronal holes.
![Morphology of Pseudostreamers and Solar Wind Properties](/assets/images/morphology-of-pseudostreamers.png)
Morphology of Pseudostreamers and Solar Wind Properties — The solar dynamo and photospheric convection lead to three main types of structures extending from the solar surface into the corona - active regions, solar filaments (prominences when observed at the limb) and coronal holes.
![Observations and Analysis of the Non-Radial Propagation of Coronal Mass Ejections Near the Sun](/assets/images/observations-and-analysis.png)
Observations and Analysis of the Non-Radial Propagation of Coronal Mass Ejections Near the Sun — The trajectories of coronal mass ejection (CME) are often observed to deviate from radial propagation from the source while within the coronagraph field of view (R <15 - 30 R_{sun}). To better understand nonradial propagation
![Current Sheets Formation in Tangled Coronal Magnetic Fields](/assets/images/current-sheets-formation.jpg)