An Instrument to Measure Coronal Emission Line Polarization

By S. Tomczyk, G. Card, T. Darnell, D. Elmore, Ron J. Lull, P. Nelson, K. Streander, J. Burkepile, R. Casini, P. Judge. 2008

239 citations recorded by the source corpus.

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

An Observational Overview of Solar Flares (2011, methodology): “Direct observations of the coronal magnetic field are also becoming possible (Linet al. 2004; Tomczyk et al. 2008).”
Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, background): “The authors compared the velocity power spectrum measured from Coronal Multi-channel Polarimeter (CoMP; Tomczyk et al. 2008) observations of quiescent coronal loops (Tomczyk and McIntosh 2009) to the chromospheric velocity power spectrum of fibrils.”
TIME–DISTANCE SEISMOLOGY OF THE SOLAR CORONA WITH CoMP (2009, background): “…measurements constrain the planeof-sky projected phase speed and therefore the transverse component of the magnetic field which is complementary to the coronal Zeeman Effect measurements (e.g. Lin, Kuhn & Coulter 2004; Tomczyk et al. 2008) which constrain the LOS component of the magnetic field.”
Origins of the Ambient Solar Wind: Implications for Space Weather (2017, methodology): “Observations of linear polarization in infrared coronal emission lines by the Coronal Multichannel Spectropolarimeter (Tomczyk et al. 2008) have demonstrated the power of such observations for establishing the topologies of magnetic structures such as flux ropes and pseudostreamers (Dove et al. 2011”