Download X-ray observations for Plan A

X-ray Solar Science
For Solar-C Plan A
Kelly Korreck
SAO
[email protected]
X-ray/EUV Science for Plan A
• Taken from the presentation on MondayGoals of Plan A
– “Understanding solar magnetic cycle”
• To look at the poles during a magnetic field
reversal
• Solar wind at the poles
• Imaging of CMEs, solar wind and CIRs
• Total solar irradiance
• Heliospheric imaging
Basic GI Characteristics
• Woltzer-1 design
– the mirrors are created as flats
• Image resolution 2.0~0.5 arc-second
• Mass ~7kg-10kg
– 45 degree sector (1/8 of a circle)
• Average grazing angle of 0.9 degrees
• 40:50 mm length of the primary and secondary
mirror
Basic Sector GI Telescope
Design
Primary Mirror
Baffle
Secondary Mirror
Sector GI Telescope Design
Mirror Bezel
Heat Shield
Mirror Segment
CAM Follower
Outer Hub Focus
Electrical
Connector
Front Flexure
CAM Plate
Inner Hub Focus
Front Support
Rear Support
X-ray Telescope
Plan A Science Goals
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Dynamo Constraints - Flux emergence in polar regions
– Combined Line Of Sight (LOS) magnetograms and X-ray observations
of jets and plumes to show the role of flux emergence vs. flux
diffusion from decaying active regions in polar activity
Down flows of meridianal flows
– Search for a coronal signature based on photospheric observations.
Deep summed exposures are likely to be needed. FOV should be full
sun for both alignment
Jet-plasma acceleration & dynamics
– X-ray Intensities using 2 analysis filters for temperature diagnostics
Sources of fast solar wind
– X-ray Intensities using 2 thin-analysis filters for temperature
diagnostics
X-ray Telescope
Plan A Science Goals (cont.)
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Polar coronal hole boundary
– Look for the interaction of closed magnetic field of the Sun with the open
magnetic field of the polar coronal hole. X-ray intensities in one filter (T~1Mk 3MK) will be necessary to find fine structure in both the quiet Sun and the polar
hole.
Flares behind the limb (Total Solar Irradiance)
– Over-the-limb flares are ideal for observing the higher-atmosphere signatures in
flares. Specifically these observations have proven useful for studying current
sheets, supra-arcade downflows, shrinking loops, and reconnection inflows.
Observations should utilize temperature responses of 3-30MK.
Active region outflows/slow solar wind origin
– Observations of outflows along loops connecting to the heliosphere. Outflows are
observed at "warm" temperatures (Fe XII-Fe XIV). Take images in 2 thinnest
filters at 60s cadence.
Transition Corona (Heliospheric Imaging)
– Deep exposures of the region from the corona to several solar radii in the EUV
with large loop structures. These observations will enable the connection
between coronal source and solar wind. Want off pointing ability to get both the
limb and the extended corona. Observations in 171 for 30 seconds to 1 minute
are needed.
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Summary of X-ray Telescope
on Plan A
• An X-ray telescope whether GI or NI will be
useful for science studies and coordinate well
with all the other instruments on the Plan A
satellite
– “Understanding solar magnetic cycle”
•
•
•
•
•
To look at the poles during a magnetic field reversal
Solar wind at the poles
Imaging of CMEs, solar wind and CIRs
Total solar irradiance
Heliospheric imaging (Transition Corona Imaging)