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These stellar outer layers can be modeled by different computer programs. Often, calculated models are used, together with other programs, to calculate synthetic spectra for stars . For example, in varying the assumed abundance of a chemical element, and comparing the synthetic spectra to observed ones, the abundance of that element in that ...
The 443.0 nm DIB is particularly broad at about 1.2 nm across - typical intrinsic stellar absorption features are 0.1 nm or less across. Later spectroscopic studies at higher spectral resolution and sensitivity revealed more and more DIBs; a catalogue of them in 1975 contained 25 known DIBs, and a decade later the number known had more than ...
Light is measured at 1.2 m above the finished floor for all areas. Work areas must have at least a value of 200 equivalent melanopic lux present for 75% or more work stations between the hours of 09:00 and 13:00 for each day of the year when daylight is incorporated into calculations.
The red color of the chromosphere could be seen during the solar eclipse of August 11, 1999.. The density of the Sun's chromosphere decreases exponentially with distance from the center of the Sun by a factor of roughly 10 million, from about 2 × 10 −4 kg/m 3 at the chromosphere's inner boundary to under 1.6 × 10 −11 kg/m 3 at the outer boundary. [7]
Early space-based imaging platforms incorporated multispectral imaging technology [1] to map details of the Earth related to coastal boundaries, vegetation, and landforms. [2] Multispectral imaging has also found use in document and painting analysis. [3] [4] Multispectral imaging measures light in a small number (typically 3 to 15) of spectral ...
Spectral optical depth or spectral optical thickness is the natural logarithm of the ratio of incident to transmitted spectral radiant power through a material. [1] Optical depth is dimensionless , and in particular is not a length, though it is a monotonically increasing function of optical path length , and approaches zero as the path length ...
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The extraterrestrial solar illuminance (E ext), corrected for the elliptic orbit by using the day number of the year (dn), is given to a good approximation by [5] E e x t = E s c ⋅ ( 1 + 0.033412 ⋅ cos ( 2 π d n − 3 365 ) ) , {\displaystyle E_{\rm {ext}}=E_{\rm {sc}}\cdot \left(1+0.033412\cdot \cos \left(2\pi {\frac {{\rm {dn}}-3 ...