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Hinode Coordinated Observations: Coronal Jets

Hinode Coordinated Observations: Coronal Jets. Standard Jet: Emerging flux reconnecting with nearby open field. Blowout Jet: Similar to bigger solar eruptions, with expulsion of cool material. Physical characteristics of coronal jets.

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Hinode Coordinated Observations: Coronal Jets

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  1. Hinode Coordinated Observations: Coronal Jets Standard Jet: Emerging flux reconnecting with nearby open field Blowout Jet: Similar to bigger solar eruptions, with expulsion of cool material Physical characteristics of coronal jets • Recently, data from the X-ray Telescope (XRT) on Hinode revealed that there are two types of coronal jets, standard and blowout (Moore et al. 2010). This work suggested that blowout jets should have components at sub-coronal temperatures. Data from the Hinode suite of instruments has been confirming these assertions and shedding new light on these features. Results provided by the SAO XRT team Contributed by the Hinode/XRT team through the Smithsonian Astrophysical Observatory

  2. Hinode Coordinated Observations: Coronal Jets Blowout jets • A blowout jet was studied in detail by Lee et al. (ApJ, 766, 1, 2013). • Helical structures in XRT and EIS are seen, indicating twisted core fields as in blowout jets. • Characteristics reminiscent of coronal mass ejections are also seen, such as an expanding cool loop seen by SOT, and coronal dimming seen by the STEREO/EUVI telescope. Helical structure indicating twisted core fields XRT image with jet and bright point (with SOT field of view) Jet and bright point Redshifts and blueshifts in EIS HII indicate helical motions EIS spectra showing jet SOT Ca II images showing cool loop expulsion Contributed by the Hinode/XRT team through the Smithsonian Astrophysical Observatory

  3. Hinode Coordinated Observations: Coronal Jets Blowout jets, cont. • Further study of a different blowout jet can be found in Young & Muglach (arXiv:1309.7324, 2013). • EIS data shows that the speed of the jet outflow is about 200 km/s. • XRT and AIA data shows multiple bright kernels at the base of the jet. • XRT filter ratios determine the temperature of the kernels to be 1.5 – 3MK, an important constraint on jet models. • Magnetic field data shows that the jet is formed on top of converging magnetic fields. EIS intensity, Doppler shift and non-thermal width XRT and AIA data showing bright kernels Photospheric magnetic field data Contributed by the Hinode/XRT team through the Smithsonian Astrophysical Observatory

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