J. Atmospheric and Solar-Terrestrial Physics 73 (10), 1214−1227, 2011
© Elsevier
Three-dimensional reconstruction of heliospheric structure using iterative tomography: A review
B.V. Jackson
Center for Astrophysics and Space Sciences, Univ. of California, San Diego, CA
P.P. Hick
Center for Astrophysics and Space Sciences, Univ. of California, San Diego, CA
San Diego Supercomputer Center, Univ. of California, San Diego, CA
A. Buffington
Center for Astrophysics and Space Sciences, Univ. of California, San Diego, CA
M.M. Bisi
Center for Astrophysics and Space Sciences, Univ. of California, San Diego, CA
Inst. of Mathematics and Physics, Aberystwyth Univ., Aberystwyth, UK
J. Clover
Center for Astrophysics and Space Sciences, Univ. of California, San Diego, CA
M. Tokumaru, M. Kojima and K. Fujiki
Solar-Terrestrial Environment Lab. (STELab), Univ. of Nagoya, Nagoya, Japan
Abstract
Current perspective and in-situ analyses using data from NASA’s twin Solar
TErrestrial RElations Observatory (STEREO) spacecraft have focused studies
on ways to provide three-dimensional (3-D) reconstructions of coronal and
heliospheric structure. Data from STEREO are proceeded by and contemporaneous
with many other types of data and analysis techniques; most of the latter
have provided 3-D information by relying on remote-sensing information beyond
those of the near corona (outside 10 RS). These include combinations of past
data from the Helios spacecraft and the Solwind coronagraphs and, continuing
from the past to the present, from observations of interplanetary scintillation
(IPS) and the Solar Mass Ejection Imager (SMEI) instrument. In this article we
review past and ongoing analyses that have led to a current great wealth of
3-D information. When properly utilized, these analyses can provide not only
shapes of CME/ICMEs but also a characterization of any solar wind structure or
global outflow.