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Energetics of the Solar Atmosphere T. Metcalf HMI Team Meeting 2003-May-1

Explore the source and triggers of coronal energization and energy release in the solar atmosphere, and analyze the role of helicity in convection and the dynamo. Use HMI data to measure energy and helicity fluxes across the photosphere.

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Energetics of the Solar Atmosphere T. Metcalf HMI Team Meeting 2003-May-1

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  1. Energetics of the Solar AtmosphereT. MetcalfHMI Team Meeting 2003-May-1 • The vector magnetic field and velocity can be used to understand the energetics of the solar atmosphere. • To measure the free energy requires chromospheric data. • But, the energy and helicity flux across the photosphere can be measured with HMI data . • With good time resolution and continuous coverage the energy and helicity input to the atmosphere can be computed.

  2. Motivation • What is the source of the coronal energization? • What triggers energy release (e.g. Flares, CME's)? Is there an energy or helicity threshold? • What is the source of helicity? What does this tell us about the convection zone and the dynamo? • Do the energy and helicity come primarily from below the photosphere or are they generated by surface motions?

  3. Poynting Flux The energy flux across the photosphere can be measured with HMI data: e.g. Kusano et al.

  4. Helicity The helicity cannot be observed, but the helicity flux across the photosphere can be: Helicity Relative Helicity See Berger & Fields, Demoulin et al., Kusano et al.

  5. Kusano's Observations Kusano et al. 2002, ApJ, 577, 501

  6. What do we need for this observation? • Vector field observations • Vector velocity observations • Good temporal resolution to resolve relevant time scales. • Good spatial resolution esp. for correlation tracking • Continuous coverage to integrate changes in the energy and helicity • HMI will be a very good instrument for these measurements.

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