SWA Normal Mode

SWA Normal mode is expected to operate for the majority of the mission, except during scheduled bursts (~5 minutes per day). Normal Mode Provides the following data products (note that LL products are listed here for convenience). Housekeeping represents 300bps which is included normal mode on the summary page but not listed explicitly here

Product	Cadence (s)	Data Rate (bps)
EAS		3239
Electron Moments	4
3D VDFs	100
Strahl Energy Shell (LL)	100
PAS		2864
Proton moments (LL)	4
3D proton & alpha VDFs	4
8s duration proton reduced VDF snapshots	300
HIS		5148
Heavy ion rates and VDFs	300
Alpha rates and VDFs	30
Total		11551

Objectives For SWA Normal Mode

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1.1.1.1 Low FIP fast wind origins (Solar Orbiter SOC Public)
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1.1.2.1 Does slow wind originate from the over-expanded edges of coronal holes? (Solar Orbiter SOC Public)
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1.1.2.2 Does slow and intermediate solar wind originate from coronal loops outside of coronal holes? (Solar Orbiter SOC Public)
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1.1.2.6 Disentangle the spatial and temporal variability of the slow wind (Solar Orbiter SOC Public)
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1.1.2.7 Trace streamer blobs and other structures through the outer corona and the heliosphere. (Solar Orbiter SOC Public)
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1.1.2.8 Determine the velocity, acceleration profile and the mass of the transient slow wind flows (Solar Orbiter SOC Public)
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1.1.3.2.1 How does the Sun's magnetic field change over time? (Solar Orbiter SOC Public)
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1.1.3.2.2 How is the heliospheric current sheet (HCS) related to coronal structure? (Solar Orbiter SOC Public)
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1.1.3.3 What is the distribution of the open magnetic flux? (Solar Orbiter SOC Public)
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1.1.4.1.3 Identify reconnection exhausts in the solar wind (Solar Orbiter SOC Public)
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1.2.1.2 Energy and mass flux in the corona. (Solar Orbiter SOC Public)
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1.2.1.9 Multi-temperature diagnostics of flaring coronal loops (Solar Orbiter SOC Public)
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1.2.2.1 Determine where energy is deposited in the solar wind (Solar Orbiter SOC Public)
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1.2.2.2 What drives the evolution of the solar wind distribution functions in situ? (Solar Orbiter SOC Public)
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1.2.2.3 What is the nature and origin of waves, turbulence and small-scale structures? (Solar Orbiter SOC Public)
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1.2.2.6 Study fast plasma flows from the edges of solar active regions discovered with Hinode/EIS (Solar Orbiter SOC Public)
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1.3.1 Solar and local origin of Alfvénic fluctuations (Solar Orbiter SOC Public)
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1.3.3 Plasma turbulence variability (Solar Orbiter SOC Public)
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1.3.4 Plasma turbulence anisotropy (Solar Orbiter SOC Public)
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2.1.1.2 CME structure (Solar Orbiter SOC Public)
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2.1.1.3 CME evolution (Solar Orbiter SOC Public)
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2.2.1 How do CMEs contribute to the global evolution of magnetic flux in the heliosphere? (Solar Orbiter SOC Public)
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2.2.2 What is the role of ICMEs in the Sun’s magnetic cycle? (Solar Orbiter SOC Public)
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2.3.2.1 Understand coronal conditions under which the shocks form and determine the interplanetary conditions where they evolve (Solar Orbiter SOC Public)
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3.1.1.2.2 Composition variations (Solar Orbiter SOC Public)
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3.1.1.6 What causes SEPs' spectral breaks? (Solar Orbiter SOC Public)
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3.1.1.7 Are there favourable environments for particle acceleration? (Solar Orbiter SOC Public)
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3.1.2.3 Flare seed particles (Solar Orbiter SOC Public)
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3.1.2.4 Explore the fact that only some of the hard X-ray peaks are related to escaping electrons, while others are not (Solar Orbiter SOC Public)
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3.1.2.5 X-ray prompt events (Solar Orbiter SOC Public)
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3.1.2.6 Delayed events (between X-ray peak and electron release time) (Solar Orbiter SOC Public)
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3.1.2.8 Explore the type III radio bursts delays (Solar Orbiter SOC Public)
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3.1.3.1 How shocks can accelerate electrons to relativistic energies (never observed for shocks near 1 AU)? (Solar Orbiter SOC Public)
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3.1.4.2 X-ray emission from electrons accelerated at CME shocks (Solar Orbiter SOC Public)
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3.2.1.1 Map the power spectrum of the turbulent magnetic field as a function of heliocentric distance in order to provide ground-truth for transport models (Solar Orbiter SOC Public)
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3.2.4 How do large and small-scale structures modulate particle fluxes? (Solar Orbiter SOC Public)
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5.10.1 What is the temporal variability of 3D thermal particle distributions? (Solar Orbiter SOC Public)
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5.10.2 How are proton and helium temperatures related to their relative drift, is there any evidence for resonant heating? (Solar Orbiter SOC Public)
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5.10.3 How common are proton beams, where do they come from and what impact do they have on ambient conditions (wave generation, heating)? (Solar Orbiter SOC Public)
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5.10.4 Identify and characterise the various forms of free energy in the particle distribution functions (Solar Orbiter SOC Public)
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5.10.5 Fully characterise the radial and latitudinal variability of 3D thermal particle distributions under different solar wind conditions (Solar Orbiter SOC Public)
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5.10.6 Electron halo population (Solar Orbiter SOC Public)
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5.10.7 How do the combined electron strahl and composition signatures vary across reconnecting solar wind current sheets? (Solar Orbiter SOC Public)
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5.4.2.1 Understand cometary properties and evolution by mapping the hydrogen Ly-α emission, proportional to the outgassing rate, along its trajectory close to the Sun (Solar Orbiter SOC Public)

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SWA Normal Mode

Objectives For SWA Normal Mode