Coronal Mass Ejections in the Declining and Minimum Phase between Solar Cycles 23 and 24

Details Coronal Mass Ejections in the Declining and Minimum Phase between Solar Cycles 23 and 24 Coronal Mass Ejections in the Declining and Minimum Phase between Solar Cycles 23 and 24

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh43a..08b&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH43A-08

Astronomy and Astrophysics

Astrophysics

[2194] Interplanetary Physics / Instruments And Techniques, [6969] Radio Science / Remote Sensing, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7900] Space Weather

Scientific paper

The Solar Mass Ejection Imager (SMEI) observes Thomson-scattered white light from heliospheric electrons across the sky all the time, and observes heliospheric structure throughout a large portion of the inner heliosphere all year round. Interplanetary scintillation (IPS) observations of velocity and g-level provide similar structure information but with sky and temporal coverage which is generally less complete. We have used Solar-Terrestrial Environment Laboratory (STELab) IPS observations to provide IPS velocity and g-level values (a proxy for density), in conjunction with our three-dimensional (3D) tomographic reconstruction program, to yield velocities and densities of the inner heliosphere out to around 3 AU. A second determination substitutes SMEI brightness information for the g-level values to derive the heliospheric density. We look at the global structure of the heliosphere throughout this time, concentrating on two time intervals from 2008 (in the declining phase of solar cycle 23). The first interval includes the 23-26 April 2008 coronal mass ejection (CME) and its interplanetary counterpart seen best in SMEI data. The second interval includes a CME (and its interplanetary counterpart) that took place 02-06 June 2008. We try to isolate the particular portion(s) of the heliosphere attributed to each event, and then estimate their masses. We also compare our results with the STEREO Heliospheric Imager data where possible.

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