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The Nov 2002 Ulysses-SOHO/UVCS Campaign Location of Ulysses:

Identifying the same very hot, highly ionised plasma (6-10 x 10 6 K) remotely at the Sun with SOHO and, after propagation, in situ at Ulysses (Poletto et al., Ap. J. Lett., 2004). The Nov 2002 Ulysses-SOHO/UVCS Campaign Location of Ulysses: Latitude = 27 o N off the west limb of the Sun

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The Nov 2002 Ulysses-SOHO/UVCS Campaign Location of Ulysses:

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  1. Identifying the same very hot, highly ionised plasma (6-10 x 106 K) remotely at the Sun with SOHO and, after propagation, in situ at Ulysses (Poletto et al., Ap. J. Lett., 2004) • The Nov 2002 Ulysses-SOHO/UVCS Campaign • Location of Ulysses: • Latitude = 27o N off the west limb of the Sun • Heliocentric distance = 4.3 AU • Solar Events: • Three large CMEs (on 19, 24, 26 Nov 2002) emitted in the general direction of Ulysses • The CMEs have probably merged by the time they reach Ulysses at 4.3 AU (1 – 2 Dec) To Ulysses 26 Nov 2002, 19:30 UT SOHO/ LASCO/C2 + EIT FeXII during the CME The black line shows the direction towards Ulysses

  2. SOHO/UVCS Observations: OVI and FeXVIII intensities vs. northern latitude at four times during and after the 26 Nov 2002 CME, at 1.7 RSUN • The Fe line is seen to increase in intensity long after the passage of the CME, i.e. at the time of post-flare loop formation • Material is cooling from a higher temperature, down through the Fe line, eventually reaching the OVI line temperature

  3. Ulysses Observations: Iron charge state vs. DOY from Ulysses/SWICS, normalized to a total flux of unity for each data sample. The normal solar wind charge state is ~10-11. The red bars at the top draw attention to intervals of unusually large enhancements in the high iron charge state Fe16+ • High Fe charge states in the solar wind are a known signature of the interplanetary counterparts of Coronal Mass Ejections (CMEs) • SOHO/UVCS has found high Fe charge states in the aftermath of CMEs close to the Sun • Here, a connection is made between the two for a specific event • The source of the high plasma temperature seems to be reconnection, high in post-flare loops

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