A New Precise Measurement of the Coronal Magnetic Field Strength

By Haosheng Lin, M. Penn, S. Tomczyk. 2000

231 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/3d1c1ea7707e2d33308c2b1f0b4c867d4b3a9f83

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Citations in the corpus

COEXISTING FLUX ROPE AND DIPPED ARCADE SECTIONS ALONG ONE SOLAR FILAMENT (2010, background): “…if these dips are associated with a twisted flux tube or an arcade, because vector magnetic fields are currently not available for the chromosphere and the corona, although attempts to measure the magnetic fields above the photosphere have been made (Judge 1998; Lin et al. 2000; Liu & Lin 2008).”
An Instrument to Measure Coronal Emission Line Polarization (2008, background): “…the nearly four decades since the detection of the Zeeman effect of the coronal green line (Harvey, 1969), coronal Zeeman measurements have not been productive until recently due to advances in the technology of near-IR detector arrays (Lin, Penn, and Tomczyk, 2000; Lin, Kuhn, and Coulter, 2004).”
Coronal loop seismology using multiple transverse loop oscillation harmonics (2007, background): “Some attempts to measure the density were undertaken (Aschwanden et al. 2003) and the average value of the magnetic field was estimated by Lin et al. (2000, 2004), but the error bars on the results are large.”
Coronal Magnetic Field Measurements (2004, background): “It was Lin et al. (2000) who first convincingly demonstrated this.”
Advances in Observing Various Coronal EUV Waves in the SDO Era and Their Seismological Applications (Invited Review) (2014, unknown): “…of the primary goals of coronal seismology, which complements other approaches including polarimetric measurements using Zeeman and Hanle effects (Lin, Penn, and Tomczyk, 2000), extrapolations of surface magnetograms (Zhao and Hoeksema, 1994; De Rosa et al., 2009), and radio observations of…”
The solar magnetic field (2006, background): “15 R above the limb for infrared emission lines from Fe XIII at λ = 1075 and 1080 nm [453].”
An Observational Overview of Solar Flares (2011, methodology): “Direct observations of the coronal magnetic field at the limbusing infrared Zeeman splitting (Lin et al. 2000) are proceeding now with the CoMP instrument(Tomczyk et al. 2008).”
Band-splitting of coronal and interplanetary type II bursts - II. Coronal magnetic field and Alfvén velocity (2002, background): “Although a big step forward was achieved recently (Lin et al. 2000) the measurements are still burdened by a low signal-to-noise ratio, low temporal and spatial resolution and can be performed only at low heights.”