An active region jet observed with Hinode

Press Release

Free access article

Issue		A&A Volume 481, Number 1, April I 2008 Science with Hinode


Page(s)		L57 - L60
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:20079081
Published online		17 January 2008

A&A 481, L57-L60 (2008)
DOI: 10.1051/0004-6361:20079081

Letter

An active region jet observed with Hinode

C. Chifor¹, P. R. Young², H. Isobe³, H. E. Mason¹, D. Tripathi¹, H. Hara⁴, and T. Yokoyama³

¹ Department of Applied Mathematics and Theoretical Physics, CMS, Wilberforce Road, Cambridge CB3 0WA, UK
e-mail: c.chifor@damtp.cam.ac.uk
² STFC Rutherford Appleton Laboratory, Chilton, Didcot, Oxfordshire OX11 0QX, UK
³ Department of Earth and Planetary Science, University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan
⁴ National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Mitaka, Tokyo 181-8588, Japan

(Received 16 November 2007 / Accepted 7 January 2008)

Abstract
Aims.We study the physical properties of an active region (AR) jet in order to probe the mechanisms responsible for it.
Methods.We report 2007 January 15/16 observations of a recurring jet situated on the west side of NOAA AR 10938. Multi-wavelength data from all three instruments onboard Hinode were analysed. This paper focuses on one instance of a jet observed with the Hinode/EUV Imaging Spectrometer (EIS). Using EIS raster data we measured the temperatures, Doppler shifts, density, and filling factor.
Results.A strong blue-shifted component and an indication of a weak red-shifted component at the base of the jet was observed around Log $T_{\rm e}$ = 6.2. The up-flow velocities exceeded 150 km s^-1. The jet component was seen over a range of temperatures between 5.4 and 6.4 in Log $T_{\rm e}$ . Using $\ion{Fe}{xii}$ $\lambda$ 186 and $\lambda$ 195 line ratios, we measured densities above Log $N_{\rm e}$ = 11 for the high-velocity up-flow component. We found that the density of the high-velocity up-flow increases with velocity. We estimate the filling factor in the jet up-flow to be <0.03. With the Hinode/Solar Optical Telescope (SOT), we observed recurrent (quasi periodic) magnetic flux cancelations just before the recurrent jet emission was seen in images taken with the X-ray Telescope (XRT).
Conclusions.The high-velocity up-flows, together with the density dependence on velocity, support an evaporation scenario for the acceleration of this jet. The high density and small filling factor, coupled with the high Doppler velocities are strongly suggestive of multiple small-scale magnetic reconnection events being responsible for the production of both EUV and X-ray jets.

Key words: Sun: activity -- Sun: corona -- Sun: flares -- Sun: magnetic fields -- Sun: -- UV radiation -- Sun: X-rays, gamma rays

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