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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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Volume 27, issue 12
Ann. Geophys., 27, 4479–4489, 2009
https://doi.org/10.5194/angeo-27-4479-2009
© Author(s) 2009. This work is distributed under
the Creative Commons Attribution 3.0 License.

Special issue: Three eyes on the Sun – multi-spacecraft studies of...

Ann. Geophys., 27, 4479–4489, 2009
https://doi.org/10.5194/angeo-27-4479-2009
© Author(s) 2009. This work is distributed under
the Creative Commons Attribution 3.0 License.

  10 Dec 2009

10 Dec 2009

3-D reconstructions of the early-November 2004 CDAW geomagnetic storms: analysis of Ooty IPS speed and density data

M. M. Bisi1, B. V. Jackson1, J. M. Clover1, P. K. Manoharan2, M. Tokumaru3, P. P. Hick1,4, and A. Buffington1 M. M. Bisi et al.
  • 1Center for Astrophysics and Space Sciences, University of California, San Diego, 9500 Gilman Drive #0424, La Jolla, CA 92093-0424, USA
  • 2Radio Astronomy Centre, National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Udhagamandalam (Ooty), 643 001, India
  • 3Solar-Terrestrial Environment Laboratory (STELab), Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8601, Japan
  • 4San Diego Supercomputer Center, University of California, San Diego, 9500 Gilman Drive #0505, La Jolla, CA 92093-0505, USA

Abstract. Interplanetary scintillation (IPS) remote-sensing observations provide a view of the solar wind covering a wide range of heliographic latitudes and heliocentric distances from the Sun between ~0.1 AU and 3.0 AU. Such observations are used to study the development of solar coronal transients and the solar wind while propagating out through interplanetary space. They can also be used to measure the inner-heliospheric response to the passage of coronal mass ejections (CMEs) and co-rotating heliospheric structures. IPS observations can, in general, provide a speed estimate of the heliospheric material crossing the observing line of site; some radio antennas/arrays can also provide a radio scintillation level. We use a three-dimensional (3-D) reconstruction technique which obtains perspective views from outward-flowing solar wind and co-rotating structure as observed from Earth by iteratively fitting a kinematic solar wind model to these data. Using this 3-D modelling technique, we are able to reconstruct the velocity and density of CMEs as they travel through interplanetary space. For the time-dependent model used here with IPS data taken from the Ootacamund (Ooty) Radio Telescope (ORT) in India, the digital resolution of the tomography is 10° by 10° in both latitude and longitude with a half-day time cadence. Typically however, the resolutions range from 10° to 20° in latitude and longitude, with a half- to one-day time cadence for IPS data dependant upon how much data are used as input to the tomography. We compare reconstructed structures during early-November 2004 with in-situ measurements from the Wind spacecraft orbiting the Sun-Earth L1-Point to validate the 3-D tomographic reconstruction results and comment on how these improve upon prior reconstructions.

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