Imaging the Solar Wind with SoloHI

Details Imaging the Solar Wind with SoloHI Imaging the Solar Wind with SoloHI

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh11b1627h&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH11B-1627

Astronomy and Astrophysics

Astrophysics

[2129] Interplanetary Physics / Interplanetary Dust, [2164] Interplanetary Physics / Solar Wind Plasma, [7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7594] Solar Physics, Astrophysics, And Astronomy / Instruments And Techniques

Scientific paper

Imaging outflows in the corona have been observed with the SOHO/LASCO instrument, since 1996. With the launch of the STEREO mission in 2006, these outflows can be followed into the heliosphere, with the SECCHI/Heliospheric Imager. For the Solar Orbiter mission, we have proposed an instrument called the Solar Orbiter Heliospheric Imager (SoloHI) to be able to image the solar wind and the density fluctuations in the wind and thus provide the link between the in-situ and remote sensing measurements. The nature of the Thomson scattering process integrates along a particular look direction but the scattering is a maximum on the Thomson sphere - the locus of points that form a right angle between the look direction and the solar vector. The experience from SECCHI/HI shows that the density fluctuations are easily visible and can be tracked back into the low corona, enabling a coupling between the solar wind plasma crossing the spacecraft and the source region in the corona. However, the SECCHI/HI observations have low cadence and long integration times. As a new observing mode for SoloHI, we have implemented a capability to readout a subset of the image at a time cadence of about 1 second. Thus small scale fluctuations can be observed in addition to the large scale fluctuations observed from SECCHI/HI. This will enable us to determine the spectral index of the density fluctuations over an unprecedented range of heights (from 5 to 135 Rsun) to compare with the in-situ determinations of the spectral index. This may indicate whether the fluctuations are generated close to the sun and convected out by the solar wind or are generated within the solar wind.

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