Engineering topics
Woo, R.
Publications and source records attributed to Woo, R..
Observational evidence for ubiquitous open magnetic field lines in the inner corona
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Ubiquitous open magnetic field lines in the inner corona
The purpose of this paper is to summarize the observational evidence for ubiquitous open magnetic field lines in the inner corona from density measurements.
On the predominance of the radial component of the magnetic field in the solar corona
In this paper, the polarized intensity measurements of the Fe XIII 10747 A line described by Arnaud are placed, for the first time, in the context of the corresponding pB images from the HAO Mauna Loa MkIII K-Coronameter, which first became available in 1980. It is shown how the predominance of the radial direction of the coronal magnetic field at solar maximum is consistent with radially expanding magnetic field lines coexisting with the large-scale structures associated with streamers.
Observational associations between the solar corona and solar interior
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Observed associations between the solar corona and solar interior
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Associating the solar wind observed by interplanetary spacecraft with the Solar Corona
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Associating observations of the sun and sola'
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Observed associations between the solar interior, corona, and solar wind
Using polarized brightness (pB) measurements made by the High Altitude Observatory (HAO) Mauna Loa Mk III K-coronameter, we investigate the daily changes of path-integrated density at1.15 R-circle dot.
Apparent Associations Between the Solar Interior, Corona, and Solar Wind
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Temperature, Density and Magnetic Field Structure of the Corona During the Total Eclipse to 1999 August 11
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Connecting the Sun and the solar wind: source regions of the fast wind observed in interplanetary space
Highly sensitive radio occultation and white light measurements of path-integrated density have shown that the solar corona comprises three distinct morphological regions, streamer, quiet Sun, and polar coronal hole, which except for the streamer region, extend radially into interplanetary space from 1.15 R***s*** to at least 30 R***s***. The authors build on these results by comparing solar wind flow speeds observed at the same time as path-integrated density.
Connecting the Sun and the Solar Wind: Latitudinal Profiles of Density and Velocity
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Connecting the Sun and the Solar Wind: Longitudinal Variations of Density and Velocity
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Temperature, Density and Magnetic Field Structure of the Corona During the Total Solar Eclipse of 11 August 1999
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Connecting the Sun and the Solar Wind: Source Regions of the Fast Wind Observed
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Connecting the Sun and the Solar Wind: I. Source Regions of the Fast Wind Observed Beyond 0.3 AU
Radio occultation and white-light measurements have shown that the solar corona comprises three distinction morphological regions in path-integrated density: streamer, quiet Sun, and polar coronal hole.