by Aerospace Corporation, National Aeronautics and Space Administration, National Technical Information Service, distributor in El Segundo, CA, [Washington, DC, Springfield, Va .
Written in English
|Statement||principal investigator, John A. Hackwell; co-investigators: James Hecht, Ronald Canterna.|
|Series||[NASA contractor report] -- NASA-CR-205677., NASA contractor report -- NASA CR-205677.|
|Contributions||Hecht, James., Canterna, Ronald., United States. National Aeronautics and Space Administration.|
|The Physical Object|
The Link Between UV Extinction and Infrared Cirrus NASA/GSFC Grant NAG5- Principal Investigator: John A. Hackwell The Aerospace Corporation P.O. Box Los Angeles, CA () Co-Investigators: James Hecht The Aerospace Corporation P.O. Box Los Angeles, CA () Ronald Canterna The University of Wyoming. Part of the NATO ASI Series book series (ASIC, volume ) Abstract Correlations between the mid infrared excess and the UV extinction parameters are investigated, using a sample of 50 stars reported to have peculiar extinction by: 1. Then, the extinction matrices as functions of the incident wavelength, incident direction, crystal size, and crystal orientation are numerically calculated for the first time. It is shown that the off-diagonal elements of the matrix are negligible. Therefore, the extinction in cirrus clouds is . Extended sources of far-infrared emission superposed on the zodiacal and galactic backgrounds are found at high galactic latitudes and near the ecliptic plane. Clouds of interstellar dust at color temperatures as high as 35K account for much of this complex structure, but the relationship to H I column density is not simple. Other features of the extended emission show the existence of warm Cited by:
For directions of sufficient reddening (E(B−V)>∼), there is a simple relation between the slope of the extinction curve in the far-UV and E(B−V).Regardless of direction, the far-UV extinction curve is proportional to 1/λ n e −2E(B−V)/λ (λ in μm, n=4), in accordance with the idea that reddened stars spectra are contaminated by scattered light (Zagury, b).Cited by: 5. The authors show that a correlation exists at high and intermediate galactic latitudes between the diffuse infrared background intensity at μm as measured by IRAS and the diffuse background. gard to the infrared spectral radiance of clouds, Fig. I shows example spectra of brightness temperature ob- served between cm -1 ( •um) and cm -1 ( •um) on Ap in the time period between and UTC. Strong absorption features by ozone at •um ( cm -1) and carbon dioxide at 15 •umCited by: The dashed lines indicate the best fits to the local residual background Infrared cirrus of x ISSA fields in this region were joined to form a mosaic covering an area more than 40across. As already mentioned, residual background subtraction is a complicated process, in general, and can introduce arbitrary errors in the measured cirrus surface brightness by: 6.
A case study of an orographic cirrus cloud observed on October 2, , over the central Andes of South America is presented with spectral BT differences up to 63K between and cm View. The final section examines recent developments involving novel techniques based on UV, x-ray, and electron beam studies. This book offers the first comprehensive overview of the spectroscopy of aerosols. It includes some results for the first time in the literature and presents a unique link between fundamental aspects and applications. The infrared cirrus are the filamentary emission seen at high galactic latitude in the IRAS data. This emission is associated with galactic interstellar clouds and was expected. The average brightness at µm is in rather good agreement with predictions based on . Abstract: The A bump is a major figure of interstellar extinction. Extinction curves with no bump however exist and are, with no exception, linear from the near-infrared down to A at least, often over all the visible-UV by: 3.