HR: 1330h
AN: SH42B-0505    [PDF]
TI: A Coronal Multi Channel Polarimeter For Magnetic Field Measurements
AU: * Darnell, T
EM: tdarnell@ucar.edu
AF: High Altitude Observatory NCAR, 3450 Mitchell Lane, Boulder, CO 80307 United States
AU: Tomczyk, S
EM: tomczyk@ucar.edu
AF: High Altitude Observatory NCAR, 3450 Mitchell Lane, Boulder, CO 80307 United States
AU: Card, G
EM: card@ucar.edu
AF: High Altitude Observatory NCAR, 3450 Mitchell Lane, Boulder, CO 80307 United States
AU: Judge, P G
EM: judge@ucar.edu
AF: High Altitude Observatory NCAR, 3450 Mitchell Lane, Boulder, CO 80307 United States
AU: Casini, R
EM: casini@ucar.edu
AF: High Altitude Observatory NCAR, 3450 Mitchell Lane, Boulder, CO 80307 United States
AU: Burkepile, J
EM: iguana@ucar.edu
AF: High Altitude Observatory NCAR, 3450 Mitchell Lane, Boulder, CO 80307 United States
AB: The Coronal Multi-channel Polarimeter (CoMP) is a filter-based polarimeter designed to provide quantitative measurements of magnetic fields in the solar corona. It will measure the Stokes parameters at the 1074.7 and 1079.8 FeXIII coronal emission lines (1.67 x 106 degrees K), and the 1083.0 nm HeI chromospheric line. The CoMP is based on a four stage birefringent filter and is designed such that the corona is imaged in two wavelengths simultaneously. The strength of the line-of-sight component of the coronal magnetic field is inferred from the measured amplitude of the Stokes V profile and an estimate of the plane-of-sky direction is made from the Stokes U/Q ratio. Further, inference of line-of-sight velocities can be made from Stokes I (red and blue wing) amplitudes. Finally, it may be possible to obtain a coronal density diagnostic capability from the ratio of the 1074.7/1079.8 amplitudes. This poster will present the latest test results as well as any preliminary data that have been obtained.
UR: http://comp.hao.ucar.edu
DE: 7509 Corona
DE: 7524 Magnetic fields
DE: 7594 Instruments and techniques
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting