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X-ray Solar Science For Solar-C Plan A

X-ray Solar Science For Solar-C Plan A. Kelly Korreck SAO kkorreck@cfa.harvard.edu. X-ray/EUV Science for Plan A. Taken from the presentation on Monday- Goals of Plan A “Understanding solar magnetic cycle” To look at the poles during a magnetic field reversal Solar wind at the poles

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X-ray Solar Science For Solar-C Plan A

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  1. X-ray Solar Science For Solar-C Plan A Kelly Korreck SAO kkorreck@cfa.harvard.edu

  2. X-ray/EUV Science for Plan A • Taken from the presentation on Monday- Goals 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

  3. 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

  4. Basic Sector GI Telescope Design Secondary Mirror Primary Mirror Baffle

  5. 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

  6. X-ray Telescope Plan A Science Goals • 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

  7. X-ray Telescope Plan A Science Goals (cont.) • 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.

  8. 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)

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