How does the solar atmosphere connect to the inner heliosphere?

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Presentation transcript:

How does the solar atmosphere connect to the inner heliosphere? Theory/modeling by Aleida Higginson (University of Michigan/NASA GSFC) How does the solar magnetic field connect from the photosphere through the corona to the inner heliosphere? How do the locations of the slow and fast solar wind map back to the Sun?

The S-Web is a feature of the heliosphere. Jet The S-Web is a feature of the heliosphere. How does the wind interact with it? Pseudostreamer /corridor Complicating factors within a dynamic, 3D heliosphere: Time evolution of surface field Solar wind propagation Expansion factor Interchange reconnection Turbulent field line spreading HCS blobs Coronal hole boundary changes Connectivity changes Flux emergence Rotation Stream interaction regions CMEs Turbulence Etc. Helmet streamer/HCS Really the s-web contains all the information  roger scott has some work to show later regarding this Courtesy X. Sun

Justin Kasper: Observations How do the plasma conditions (e.g. composition, charge states) change with height and wind speed? At what height(s) is the Alfven critical point in slow and fast solar wind flows? Justin Kasper: Observations Low speeds: Helium abundance strongly correlated with solar cycle. Correlation decreases with increasing speed. Suggests the variation is due to changes at the source region (corona). Role of Coulomb collisions? PERCENT He/H

Preferential Heating Zone Estimate number of Coulomb thermalization times from corona to spacecraft. Ratio of Proton T /T , & Helium-proton temperature ratios vs. speed ~same as vs. ‘Coulomb number’ PSP will fly through Preferential Heating Zone Coulomb Number Speed km/sec Kasper et al. 2017

Parker Solar Probe will sample below the Alfven critical point Discussion Included Heating and acceleration are likely two different processes. The slow solar wind likely has multiple sources / populations. Immediate benefits from Parker Solar Probe: Higher confidence in mapping and less contamination from propagation – hovering over a single source region on the Sun! Questions What are the in situ signatures associated with crossing any S-Web / Q-map arc? (Use Probe / Helios / Ulysses) What does the imprint of the S-Web solar wind look like in the solar wind after affected by dynamic processes? Needed: Far side / polar field magnetic field observations and Your ideas! TODAY: Connecting Slow Solar Wind Theories to Observations (Arge)