Comparison of infrared radiometrie, observed and sunshine‐derived cloud cover

Harrison, A. W.; Coombes, Charles A.

doi:10.1080/07055900.1986.9649252

Cited by 3 publications

(1 citation statement)

References 7 publications

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“…As the density of a cloud increases, the cloud becomes visibly opaque just before becoming opaque to infrared radiation. Harrison and Coombes (1986) showed that infrared estimates of cloud cover are closer to visual estimates of total opacity than to those of total amount; hence it should be assumed here that cloud cover C refers to total opacity rather than to total amount. (See Manual of Surface Weather Observations, (AES, 1977) for definitions of total opacity and total amount.)…”

Section: Data Basementioning

confidence: 99%

Calibration of a three‐component angular distribution model of sky radiance

Coombes

Harrison

1988

Atmosphere-Ocean

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Section: Data Basementioning

confidence: 99%

Calibration of a three‐component angular distribution model of sky radiance

Coombes

Harrison

1988

Atmosphere-Ocean

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CME Theory and Models

et al. 2006

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This chapter provides an overview of current efforts in the theory and modeling of CMEs.Five key areas are discussed: (1) CME initiation; (2) CME evolution and propagation; (3) the structure of interplanetary CMEs derived from flux rope modeling; (4) CME shock formation in the inner corona; and (5) particle acceleration and transport at CME driven shocks. In the section on CME initiation three contemporary models are highlighted. Two of these focus on how energy stored in the coronal magnetic field can be released violently to drive CMEs. The third model assumes that CMEs can be directly driven by currents from below the photosphere. CMEs evolve considerably as they expand from the magnetically dominated lower corona into the advectively dominated solar wind. The section on evolution and propagation presents two approaches to the problem. One is primarily analytical and focuses on the key physical processes involved. The other is primarily numerical and illustrates the complexity of possible interactions between the CME and the ambient medium. The section on flux rope fitting reviews the accuracy and reliability of various methods. The section on shock formation considers the effect of the rapid decrease in the magnetic field and plasma density with height. Finally, in the section on particle acceleration and transport, some recent developments in the theory of diffusive particle acceleration at CME shocks are discussed. These include efforts to combine self-consistently the process of particle acceleration in the vicinity of the shock with the subsequent escape and transport of particles to distant regions.

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