Solar Wind Compositional Variability and the Need for an Ultra-High Temporal Resolution Mass Spectrometer: Introduction to the Helical Ion Path Spectrometer (HIPS)

Details Solar Wind Compositional Variability and the Need for an Ultra-High Temporal Resolution Mass Spectrometer: Introduction to the Helical Ion Path Spectrometer (HIPS) Solar Wind Compositional Variability and the Need for an Ultra-High Temporal Resolution Mass Spectrometer: Introduction to the Helical Ion Path Spectrometer (HIPS)

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh43a..18a&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH43A-18

Physics

7507 Chromosphere, 7513 Coronal Mass Ejections, 7531 Prominence Eruptions, 7537 Solar And Stellar Variability, 7594 Instruments And Techniques

Scientific paper

Solar wind composition measurements serve as an indicator of the sub-coronal and coronal processes responsible for the formation of these heliospheric features. While current state-of-the-art instrumentation have identified temporal variations in solar wind/CME composition on the order of 10's of minutes, these detections have occurred during relatively quiescent periods when temporal variations of the collective solar wind (including magnetic field variations) occur over periods in excess of the current minimum instrumental duty cycle of 5-minutes. Consequently, the compositional markers of the microphysics responsible for the formation of highly variable solar wind flows and for CME/prominence formation remain overlooked. The development of a novel ultra-high temporal resolution ion mass spectrometer utilizing a helical ion path time-of-flight (TOF) system within a compact, low-mass, low-power instrument has been undertaken in order to address the need for temporally enhanced solar wind composition measurements. The Helical Ion Path Spectrometer (HIPS) is designed specifically to measure solar wind heavy ion plasma from 3He+2 ≤ M/q ≤ Fe+6 and 0.6-20.0 keV/q with an order of magnitude greater geometric factor than current solar wind ion mass spectrometers, and produce 1-10 ms mass spectra with a mass resolution of M/ΔM ~ 200 or greater, all within a duty cycle of ≤ 90-s. The temporal resolution of HIPS is sufficient to probe solar wind and CME spatial/temporal dimensions down to an ion gyroradius in solar wind flow boundaries at 1 AU. We present evidence supporting the need for greater temporal resolution solar wind composition measurement through an overview of solar wind mass spectroscopy results to date, and an introduction to the HIPS mass spectrometer instrument concept.

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