Small-scale X-ray/EUV Jets seen in Hinode XRT and TRACE

Details Small-scale X-ray/EUV Jets seen in Hinode XRT and TRACE Small-scale X-ray/EUV Jets seen in Hinode XRT and TRACE

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh53a1061k&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH53A-1061

Mathematics

Logic

7509 Corona, 7526 Magnetic Reconnection (2723, 7835), 7546 Transition Region, 7549 Ultraviolet Emissions, 7554 X-Rays, Gamma Rays, And Neutrinos

Scientific paper

In this study, we present the morphological and kinematic characteristics of three small-scale X-ray/EUV jets that are simultaneously observed by the X-ray telescope (XRT) onboard Hinode (Solar-B) and the TRACE. For this study, we examined all XRT movies with a thin Al/Poly filter from 2006 October 20 to April 8 to look for small-scale X-ray eruptions and then found 34 eruptions. Next we took a look at the corresponding TRACE 171/195 {Å} images associated with these X-ray eruptions. As a result, we found three simultaneous X-ray and EUV jets and their major characteristics can be summarized as follows : (1) They all have no association with major flares. (2) From the comparison between XRT and TRACE observations, we found that they have similar characteristics in terms of projected speed, lifetime, and size. (3) Their sizes range from 4 × 105 to 5 × 105 km. (4) Their projected speeds are estimated to be 180-310 km s-1 with an average speed of about 250 km s- 1 (5) Their lifetimes lie in the range of 100 to 600 s. (6) From the comparison between the XRT images with the SOHO MDI maps for two events, all they are associated with the parasitic polarity region. These characteristics are similar to the previous observations for X-ray jets by the Yohkoh SXT but quite different from EUV jets associated with Hα surges. In addition, from the EIS four spectral lines for the last event, we found blueshift (up to -64 km s-1) and redshift (up to 20 km s-1) motions as well as nonthermal velocities ranging from 57 to 106 km s-1 at the jet footpoint. We note a tendency : the hotter the maximum ionization temperature is, the larger the area of blueshift region is. These characteristics are consistent with a typical jet model that includes the magnetic reconnection between open coronal fields and emerging magnetic fields.

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