Articles | Volume 26, issue 2
Ann. Geophys., 26, 213–229, 2008

Special issue: 3rd European Space Weather Week (ESWW)

Ann. Geophys., 26, 213–229, 2008

  26 Feb 2008

26 Feb 2008

Magnetic clouds seen at different locations in the heliosphere

L. Rodriguez1, A. N. Zhukov2,1, S. Dasso4,3, C. H. Mandrini3, H. Cremades5, C. Cid6, Y. Cerrato6, E. Saiz6, A. Aran7, M. Menvielle8, S. Poedts9, and B. Schmieder10 L. Rodriguez et al.
  • 1Solar Influences Data analysis Center, Royal Observatory of Belgium, Brussels, Belgium
  • 2Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, Russia
  • 3Instituto de Astronomía y Física del Espacio, CONICET-UBA, Buenos Aires, Argentina
  • 4Departamento de Física, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Buenos Aires, Argentina
  • 5NASA Goddard Space Flight Center, Greenbelt, MD, USA
  • 6Universidad de Alcala, Madrid, Spain
  • 7Universitat de Barcelona, Spain
  • 8Centre d'étude des Environnements Terrestre et Planétaires, Vélizy, France
  • 9K.U. Leuven, Leuven, Belgium
  • 10Observatoire de Paris, Meudon, France

Abstract. We analyze two magnetic clouds (MCs) observed in different points of the heliosphere. The main aim of the present study is to provide a link between the different aspects of this phenomenon, starting with information on the origins of the MCs at the Sun and following by the analysis of in-situ observations at 1 AU and at Ulysses. The candidate source regions were identified in SOHO/EIT and SOHO/MDI observations. They were correlated with H-α images that were obtained from ground-based observatories. Hints on the internal magnetic field configuration of the associated coronal mass ejections are obtained from LASCO C2 images. In interplanetary space, magnetic and plasma moments of the distribution function of plasma species (ACE/Ulysses) were analyzed together with information on the plasma composition, and the results were compared between both spacecraft in order to understand how these structures interact and evolve in their cruise from the Sun to 5 AU. Additionally, estimates of global magnitudes of magnetic fluxes and helicity were obtained from magnetic field models applied to the data in interplanetary space. We have found that these magnetic characteristics were well kept from their solar source, up to 5 AU where Ulysses provided valuable information which, together with that obtained from ACE, can help to reinforce the correct matching of solar events and their interplanetary counterparts.