Inversion of the zodiacal infrared brightness integral

1987 ◽  
Vol 320 ◽  
pp. 928 ◽  
Author(s):  
S. S. Hong ◽  
I. K. Um
Keyword(s):  
Infrared Brightness

Infrared brightness of a comet belt beyond Neptune

1988 ◽  
Vol 42 (1) ◽  
pp. 41-47 ◽  
Author(s):  
A. A. Jackson ◽  
R. M. Killen
Keyword(s):  
Infrared Brightness

scholarly journals Efficient radiative transfer model for thermal infrared brightness temperature simulation in cloudy atmospheres

2020 ◽  
Vol 28 (18) ◽  
pp. 25730
Author(s):  
Wenwen Li ◽  
Feng Zhang ◽  
Yi-Ning Shi ◽  
Hironobu Iwabuchi ◽  
Mingwei Zhu ◽  
...  
Keyword(s):  
Radiative Transfer ◽  
Brightness Temperature ◽  
Thermal Infrared ◽  
Radiative Transfer Model ◽  
Transfer Model ◽  
Infrared Brightness

Far-Infrared Brightness Temperatures of the Planets

1972 ◽  
Vol 178 ◽  
pp. L89 ◽  
Author(s):  
K. R. Armstrong ◽  
D. A., Jr. Harper ◽  
F. J. Low
Keyword(s):  
Far Infrared ◽  
Brightness Temperatures ◽  
Infrared Brightness

scholarly journals Barred Extreme IRAS Galaxies

1996 ◽  
Vol 157 ◽  
pp. 256-258
Author(s):  
Wim van Driel ◽  
Bert van den Broek
Keyword(s):  
Star Formation ◽  
Massive Star ◽  
Formation Rate ◽  
Far Infrared ◽  
Radio Continuum ◽  
Massive Star Formation ◽  
Barred Galaxies ◽  
Interacting Systems ◽  
Isolated Systems ◽  
Infrared Brightness

AbstractWe studied a statistically complete sample of 57 southern socalled extreme IRAS galaxies, i.e., objects with a high far-infrared/blue luminosity ratio, LFIR/LB>3, using optical (imaging and spectra), radio continuum, and CO(1–0) line observations. The sample can be divided into three distinct categories: dwarfs (20%), barred spirals (35%), and interacting systems (35%). The barred galaxies are generally morphologically undisturbed, isolated systems, with average star formation rates (4 M⊙ yr–1) and efficiencies (LFIR/MH2 = 16 L⊙/M⊙) for galaxies in our sample. An enhanced massive star formation rate is the cause of the infrared brightness in 93% of all galaxies in the sample. The nuclear region is the most important star formation locus, generally unresolved at 1" resolution, i.e., less than 0.2-0.6 kpc size (H0=75 km s–1 Mpc–1), though 2 kpc size in three cases. In about two-thirds of the extreme IRAS SB’s, fainter, diffuse (2.5-10 kpc size) massive star formation is seen in the bar as well.

How microphysical choices affect simulated infrared brightness temperatures

2015 ◽  
Vol 156 ◽  
pp. 67-79 ◽  
Author(s):  
S. Eikenberg ◽  
C. Köhler ◽  
A. Seifert ◽  
S. Crewell
Keyword(s):  
Brightness Temperatures ◽  
Infrared Brightness
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