1 / 3

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

kane
Télécharger la présentation

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

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related