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CME observations using spectroscopy and polarimetry

CME observations using spectroscopy and polarimetry. Hui Tian, Scott W. McIntosh, Steven Tomczyk, Christian Bethge, Giuliana de Toma, Leonard Sitongia, Don Kolinski, et al. HINODE/EIS & CoMP observations. Spectroscopic observations of CMEs.

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CME observations using spectroscopy and polarimetry

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  1. CME observations using spectroscopy and polarimetry Hui Tian, Scott W. McIntosh, Steven Tomczyk, Christian Bethge, Giuliana de Toma, Leonard Sitongia, Don Kolinski, et al. HINODE/EIS & CoMP observations

  2. Spectroscopic observations of CMEs

  3. The background corona and CME ejecta can be separated through spectroscopic observations • Plasma properties (density, temperature) and real speed of CMEs (v=Sqrt(vpos2+vlos2)) can be derived • Mass of the ejecta can be estimated Tian, McIntosh et al. 2012, ApJ, 748, 106

  4. CoMP: Coronal Multi-channel Polarimeter • Locations • Mauna Loa Solar Observatory: almost daily observations since October 2010 • Spectral sampling: • Fe XIII 1074.7/1079.8 nm and He I 1083.0 nm • Images of each polarization state at 3 or 5 spectral positions • FOV: 1.05 to 1.4 Rsun • Spatial Resolution: 4.46”/pixel • Cadence: typically 30 s or 50 s Tomczyk et al. 2008, Sol. Phys.

  5. CoMP observations of solar eruptions

  6. EUV waves produced by halo-CMEs • CoMP provides simultaneous high-cadence (30 s) observations of coronal line intensity, Doppler shift and line width for the first time. • Solar eruptions are associated with dramatic changes of Doppler shift and line width.

  7. Density map of the corona and CME mass • Density: from ratio of Fe XIII 1074.7/1079.8 nm • Estimate CME mass • Calculate coronal magnetic field strength From CHIANTI 7.0 Preliminary results data correction not finalized

  8. Stokes Q, U, V • Circular Polarization (V): LOS magnetic field strength from longitudinal Zeeman effect • Linear Polarization (Q,U) from resonance scattering effect • Degree of linear polarization (Ltot/I) • Azimuth of B (POS magnetic field direction) Ltot=(Q2+U2)1/2 ϕ=0.5 atan (U/Q)

  9. Summary • Spectroscopic observations (HINODE/EIS, IRIS, et al.) can be helpful in studies of (especially halo-) CME plasma properties, LOS kinematics, development and recovery of dimmings. • Simultaneous observations of electron density, LOS Doppler shift, line width and linear/circular polarization by CoMP can be used to constrain models of CME initiation and propagation. • We need COSMO+ChroMag. Observations of halo-CMEs by ground-based instruments like COSMO and ChroMag provide a cheap and low-risk means of space weather monitoring. Posters 086 & 090

  10. Post-CME dynamics

  11. Dec 14-15 2006 CME May 19 2007 CME • A small portion of the plasma in the dimming region is flowing outward at a speed of ~100 km/s. These outflows could potentially play an important role in refilling of the corona, mass supply to the solar wind, and additional acceleration of CMEs • Spectroscopic observations can provide a measurement of the density change and thus can be used to estimate mass of CMEs, especially halo-CMEs (mass loss in dimming)

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