Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsh32a..07l&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #SH32A-07
Astronomy and Astrophysics
Astrophysics
[2101] Interplanetary Physics / Coronal Mass Ejections, [2139] Interplanetary Physics / Interplanetary Shocks, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections
Scientific paper
We analyze the dynamics of interplanetary coronal mass ejections (ICMEs) through the interplanetary medium from the lower solar corona to near 5.3 AU. Our analysis uses a hydrodynamical one-dimensional model derived from the fluid equation of motion that considers an effective drag force under both the laminar and turbulent hypotheses (low and high Reynolds number, respectively). The model has three types of input parameters. The first set is related to the ICME itself, i. e., initial speed and mass; the second set of parameters is related to the ambient solar wind: density and velocity; and the final set corresponds to the ambient solar wind - ICME interaction: an ICME expansion factor and a viscosity or drag parameter. We utilize this model to explain the radial dynamics of a particular ICME detected at three different locations:Close to the Sun, where the ICME was ejected on January 20th, 2004 by the SOHO/LASCO coronographs; two days later, at Earth's L1 by the ACE spacecraft ~1 AU, and finally, ~14 days later, at ~5.3 AU by the Ulysses spacecraft near Jupiter's orbit. The model is then compared to a general set of ICMEs data from Ulysses that cover distances from ~1.3 AU to ~5.3 AU. Our model successfully reproduces the dynamic behavior of ICMEs at distances near Earth's orbit and works reasonably well at larger distances near ~5.3 AU. Therefore, our analysis shows that the ICME - solar wind interaction may be treated as a drag interaction with the appropriate drag factors, not only inside one astronomical unit, but at larger distances. Finally, we show that our model is useful in identifying ICMEs at different heliocentric distances.
Borgazzi Andrea
Flandes Alberto
Lara Alejandro
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