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DKIST Coronal Spectroscopy: The Missing Link in Coupling the Sun and Heliosphere

Learn about the latest advancements in linking the Sun and Heliosphere through comprehensive plasma measurements in the "gap" between disk-imagers and outer-field coronagraphs. Explore upcoming programs like DKIST employing new coronagraphy and spectroscopy combinations to enhance data analysis, atomic physics effects, and 3D coronal magnetic field measurements. Dive into the trade-offs between global and small field-of-view instruments and the potential of new off-limb emission lines for better physics probing. Discover insights from expert talks and poster summaries at the session.

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DKIST Coronal Spectroscopy: The Missing Link in Coupling the Sun and Heliosphere

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  1. SHINE 2017 Session 8 DKIST Coronal Spectroscopy: The Missing Link in Coupling the Sun and Heliosphere Progress & Prospects Report Organizers: SteveCranmer(CU Boulder) Mari Paz Miralles (SAO) Valentín Martínez Pillet (NSO) Scott McIntosh (HAO)

  2. Session 8 Goals & Questions • In order to test/validate theoretical models, we need comprehensive measurements of plasma in the “gap” between disk-imagers & outer-field coronagraphs. • Upcoming programs (e.g., DKIST) will employ new combinations of inner-field coronagraphy & spectroscopy. Here we explore what they’ll do and how they’ll help us answer long-standing questions. Do we understand the data analysis challenges in converting measurements into useful constraints on models/theory? What computational tools are needed to make best use of the coming flood of data? Do we understand the atomic physics effects well enough to be able to improve 3D coronal magnetic field measurements? What are the tradeoffs between global coronagraphs (e.g., CoMP, COSMO) andsmall field-of-view, high-throughput instruments (Cryo-NIRSP on DKIST) ? To what extent can “new” off-limb emission lines be used to better probe physics?

  3. Schedule 2:00 – 3:15: • Brief introduction from session organizers (this!) • Scene-setting talk #1: Laurel Rachmeler, NASA/MSFC:“Challenges in Spectro-polarimetric Measurements ofthe Coronal and Chromospheric Magnetic Field”

  4. Remote sensing the invisible

  5. Observations of solar B. Bits and pieces of the puzzle everywhere

  6. Observations of solar B. Bits and pieces of the puzzle everywhere “We’d like to ingest all these [incomplete] measurements into an amazing piece of code...”[to get full B(x,y,z,t)]

  7. The magnetic field parameter is entangled with plasma parameters The magnetic field changes on space/time scales smaller than the observations Estimation of the true error of the inversion involves many sources, some not easily quantifiable. All-around Challenges

  8. The magnetic field parameter is entangled with plasma parameters The magnetic field changes on space/time scales smaller than the observations Estimation of the true error of the inversion involves many sources, some not easily quantifiable. All-around Challenges “...backing into the chromosphere slowly... it’s a very scary place.”--- Tim Bastian

  9. Schedule 2:00 – 3:15: • Brief introduction from session organizers (this!) • Scene-setting talk #1: Laurel Rachmeler, NASA/MSFC:“Challenges in Spectro-polarimetric Measurements ofthe Coronal and Chromospheric Magnetic Field” • Poster summaries: Judit Szente (AwSOM), Paul Song (theory)

  10. Schedule 2:00 – 3:15: • Brief introduction from session organizers (this!) • Scene-setting talk #1: Laurel Rachmeler, NASA/MSFC:“Challenges in Spectro-polarimetric Measurements ofthe Coronal and Chromospheric Magnetic Field” • Poster summaries: Judit Szente (AwSOM), Paul Song (theory) 3:15 – 3:45: • Coffee break 3:45 – 5:00: • Scene-setting talk #2: Jeff Kuhn, U. Hawaii:“DKIST Coronal Spectroscopy: Getting ready for 2020” • Poster summaries: Chris Gilbert (theory), Jonathan Darnel (GOES-16/SUVI), Laurel Rachmeler (CLASP2) 5:00 – ???: • Poster session with refreshments

  11. Wanted: Coronal Photons DKIST 4.2m IRIS, AIA, COMP 0.2m SOLARC (Haleakala) 0.45m COMP (proposed) 1.5m DKIST: between 10 and 400 times more coronal flux 4m → 105 photons / coronal line / arcsec2 / second

  12. Why Haleakala, why the infrared? Pukalani Haleakala at 4μ & everywhere else? Haleakala “as good as going to space!”

  13. The IR sky, Coronal wavelengths, discovery science Sky and Corona at 0.1R (2R) 1994 Temperature sensitivity from 3000K to 3MK

  14. Lively discussion . . . • Poster contributions on 3D models, new heating mechanisms, & new instrument concepts. • We need better data, better analysis, & better models (*) for interpretation:all in parallel?! (*) Beware: different definitions for “model” exist • Eventually, improved 3D B-field measurements can feed into space weather forecasting models. Data assimilation? • Despite the challenges, there was a lot of optimism! • NSO will be hosting workshops to develop DKIST Science Use Cases in preparation for first light (2020).

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