![]() ![]() Therefore, the effective IFOV of the MSS detector in the cross-track direction was considered to be 68 meters which corresponds to a nominal picture element (pixel) ground area of 68 by 83 meters at the satellite nadir point. The sample taken at this instant represented 15 meters of previous information and 68 meters of new information. After 9.958 microseconds, the 83 by 83 meter image has moved 67.9 meters. The scan monitor sensor ensures that the cross-track optical scan is 185 km at nominal altitude regardless of mirror scan nonlinearity or other perturbations of mirror velocity.Ĭross-track image velocity was nominally 6.82 meters per microsecond. To understand this concept consider a ground scene composed of a single 83 by 83 meter area. Landsat 3 carried an MSS sensor with an additional band, designated band 8, that responded to thermal (heat) infrared radiation.Īn MSS scene had an Instantaneous Field Of View (IFOV) of 68 meters in the cross-track direction by 83 meters in the along-track direction (223.0 by 272.3 feet respectively). The first five Landsat satellites carried the MSS sensor which responded to Earth-reflected sunlight in four spectral bands. Bohrs model calculated the following energies for an electron in the shell, n. The forward motion of the satellite provided the along-track scan line progression. Bohrs model of hydrogen is based on the nonclassical assumption that electrons travel in specific shells, or orbits, around the nucleus. The cross-track scanning was accomplished by an oscillating mirror six lines were scanned simultaneously in each of the four spectral bands for each mirror sweep. Springer, Berlin (1955).The Multispectral Scanner (MSS) sensors were line scanning devices observing the Earth perpendicular to the orbital track. Advanced treatment of radiative transfer with astrophysical applications University Science Books, Mill Valley (1991). ionized Helium, which requires a very high temperature for its formation. Shu, F.H.: The Physics of Astrophysics, vol. For stellar spectra, the absorption lines represent how much light is removed. Good discussion of TE equations, absorption and emission coefficients, and radiative transfer Rybicki, G.B., Lightman, A.P.: Radiative Processes in Astrophysics. Certainly the existence of such striking features as the dark spectral lines that break up the spectra of stars implies the presence of absorption processes that operate in a highly selective manner. Basic text of thermodynamics and statistical physics, including a good discussion of TE equations Reif, F.: Fundamentals of Statistical and Thermal Physics. Tables with oscillator strength values for lines of astrophysical interest. Morton, D.C., Dinerstein, H.L.: Astrophys. Includes problems related to line formation in atmospheres and expanding envelopes However, an adequate theory of line-formation, including non-l.t.e. Discussion on radiative transfer in stellar atmospheres and spectral line profiles. According to theories of model stellar atmospheres only stars of spectral types from. Introduction to stellar structure and evolution, including a discussion on the main radiation field concepts, such as intensity and flux ![]() Maciel, W.J.: Introdução à Estrutura e Evolução Estelar. Includes basic equations of TE, Einstein coefficients definitions, and references to original works Complete treatment of spectral line formation in astrophysical conditions and broadening processes Jefferies, J.T.: Spectral Line Formation. Other tabulations may be found in Harris, D.L. Includes tables for the Hjerting function under several conditions. Tables of the line broadening function H(a,v). Includes detailed tables of atomic and molecular dataįinn, G.D., Mugglestone, D.: Mon. American Institute of Physics, New York (1996). Drake, G.W.F.: Atomic, Molecular and Optical Physics Handbook. ![]()
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