Maria S' Madjarska

1
X-ray/EUV jet in EIS, SUMER, STEREO and XRT data
temperatures and dynamics
Maria S. Madjarska Max-Planck Institute for
Solar System Research, Max-Planck Str. 2,
Katlenburg-Lindau, Germany Armagh Observatory,
College Hill, Armagh BT61 9DG, N. Ireland
Intro Soft X-ray jets are phenomena happening
in the solar corona and were discovered by the
SXT aboard Yohkoh. Occur in BPs and active
regions and were associated with region of mixed
magnetic polarities or a sattelite polarity
region. From 2D MHD simulations Yokoyama
Shibata (1995, 1996) suggested that the velocity
of the hot plasma flow is 800-1000 km/s.
However, the range of the velocities observed by
Yohkoh is 10-1000 km/s with an average of 200
km/s. From EIS slot observations Culhane et al.
(2007) derived the temperature interval during a
jet in the range 0.4 MK 5.0 MK.
Spectrscopic imager data - EIS/Hinode
raster image in spectral lines covering the
temperature range 0.25 MK (O V) 2.5 MK (Fe
XVI), 2" 512" - SUMER sit-and-stare, 10 000 K
(C I) 1.0 MK (Mg X)? - SECCHI A B Fe IX/X
171 Å - XRT/Hinode Al-poly
What more can we learn from the simultaneous
spectroscopic imager observations?
? The dynamics temporal evolution, Doppler
shifts, true velocity
S II Si II Ci
CI
Fe XII
? The temperatures
O VI
O V
Fe XII
Fe XIII
Fe XI

• We found
• Doppler shifts up to 420 km/s which give us a
  t rue velocity of 700 750 km/s
• Temperatures - 0.2 MK (N V 1238) 2.5 MK (Fe
  XV)? multi-temperature structure cooler
  downflows along a loop and hotter upflows (i.e.
  the jet)
• Dynamics talk to Maria about it .