The figure below shows what stellar spectra are like in this wavelength range. All stars hotter than about 3000 K effective temperature radiate like a hot blackbody at these long wavelengths, possibly with a very few atomic lines (of Hydrogen, in the A-type stars) or molecular bands (the CO band overtone near 2.25 microns for example, in K-type stars and G-type stars). ... unusual features: mixed chemistry sources, Wolf-Rayet stars, ice bands, featureless carbon-star spectra ...

Microsymposium 34, MS058, 2001 ANOMALIES OF THE MOON'S THERMAL EMISSION IN THE IR SPECTRAL RANGE (10.5 - 12.5 micron). ... Sternberg State Astronomical Institute, Moscow, 119899, Russia, pugach@sai.msu.ru Summary: New satellite measurements of the lunar-surface radiation temperature were used to construct the spatial angular function of thermal radiation of the Moon in the infrared (10.5-12.5 micron) spectral range. ... These thermal anomalies are observed only in the limited range of phase angles. ...

... Unequal distribution of radiation due to earth axis tilt is the ultimate driver of the weather." You first have to distinguish between incoming solar radiation (visible wavelengths) and outgoing longwave (infrared wavelengths) radiation due to the earth's finite (above absolute zero) temperature. Secondly, even if the earth's axis tilt would be zero, unequal distribution of incoming solar radiation would still occur, due to the fact that the earth is *ROUND*! ...

... Credit: G. S. Orton P. A. Yanamandra-Fisher ( JPL ), Keck Observatory , NASA Explanation: This strange, false-color image of otherwise familiar planet Saturn shows temperature changes based on thermal infrared emission in the gas giant's atmosphere and rings. ... But a surprising result of the infrared image data is the a clear indication of an abruptly warmer polar cap and bright hot spot at Saturn's south pole. ... Publications with keywords: infrared - Saturn - south pole . ... Crescent Saturn . ...

The hotbed effect (hothouse effect) in the planets atmosphere is the inside atmosphere layers heating (of the Earth, Venus etc.), due to the transparent planet atmosphere for the main part of solar radiation (in optical range). In the atmosphere of the Earth this radiation is absorbed by the molecules of H2O, C02, O3 and others. ... As a result of human activities the CO2 content is increasing (and the other gases, absorbing in infrared range). ...

... 2005 February 10 . Red Saturn . Credit: G. S. Orton P. A. Yanamandra-Fisher ( JPL ), Keck Observatory , NASA . ... Recorded from the Keck I telescope on Mauna Kea , the sharp, ground-based picture of Saturn's southern hemisphere is a mosaic of 35 images. ... But a surprising result of the infrared image data is the a clear indication of an abruptly warmer polar cap and bright hot spot at Saturn's south pole. ... So how hot is Saturn's hot spot? ... About APOD | ... NASA Official: Jay Norris. ...

Next: Antenna gain considerations and Up: Some theory Previous: Some theory . To provide correct flux density units for the visibilities, , from an interferometer, the measured correlation coefficient at the correlator ( ) needs to be scaled by a system temperature and a telescope sensitivity factor ( ). ... For a zenith opacity , observing at an elevation of , and if the atmosphere is approximated as having a uniform temperature , then the atmospheric contribution to system temperature is . ...

... In brief: the frequency-dependent radiative transfer equation is solved for a dust under assumption of spherically-symmetric geometry for its distribution taking into account particle size distribution and quantum heating effects for the very small dust particles. ... Table: Model parameters for IRAS04296+3429. ... parameter . ... hot dust shell) . ... The best fit to the spectral energy distribution of IRAS04296 is shown by heavy solid line (see Table2 for details concerning parameters of the model...

INFRARED FOURIER-SPECTROMETER SICH-F . ... Instrument work regimes: 1) Inside. 2) Calibration at inside standard sources 2 - 4 times per a rotation. 3) Calibration at "free space" 2 - 4 times per a rotation. 4) Infrared radiation measuring 10 - 40 min. per a rotation. ... Spectrometer consists of the photodetector block and the block of signal processing and control. ... Diagnostic information and attach data will transfer by state telemetric channels. ... Detector temperature. ...

... Because of the Earth 's gravity, atmosphere is horizontally stratified (see, e.g., Kelley, 1989). Its structure can be organized by using the neutral gas temperature, as shown in the figure from mid-latitudes (note the logarithmic altitude scale). When going upward from the ground within the lowermost atmospheric region, troposphere, the temperature decreases up to about 10 km altitude (tropopause). ... Here the radiation also ionizes the neutral atmosphere, creating the ionosphere . ... 1989. ...

Next: Direct Monitoring of T Tauri Stars Previous: X--ray Activity and PMS Stars . Pointed EINSTEIN observations of TTs in the Taurus--Auriga star forming region (SFR) detected five serendipitous sources in the field (Feigelson & Kriss 1981 and Walter & Kuhi 1981). ... Walter (1986) called these objects naked T Tauri stars (nTTs; Walter 1986, Walter et al . ... The catalog of Herbig & Bell (1988) distinguished between cTTs and weak--lined T Tauri stars (wTTs) instead of nTTs. ...

... Tonight's Sky . ... Observing . ... Sky this Month . ... Observing Podcasts . ... Astronomy for Kids . ... Titan's temperature lag . ... The latitude banding has been smoothed to more clearly show the how Titan's peak temperature moves from 19 degrees south to 16 degrees north latitude between 2004 and 2016. ... Only registered members of Astronomy.com are allowed to comment on this article. ... Receive news, sky-event information, observing tips, and more from Astronomy's weekly email newsletter. ...

Observation and modelling of main sequence star chromospheres. ... We compare our calculations to recent high res­ olution observations for selected stars in a narrow spectral range ((R­I) џ =0.875\Sigma0.05); we show that Hff line profiles behave as expected, with a tight correlation be­ tween the line width and equivalent width. ... We show that the hydrogen series dominate the radiative cooling in the spectral lines (form 40% to 90%) for Hff emission line stars. ...

... The variability of the spectrum of the optical component of the IR-source IRAS01005+7910 was discovered for the first time in the BTA spectra [1]. ... The spectral features include absorptions that form in near-photospheric layers, narrow envelope emissions, and emission-absorption profiles that form in photosphere-to-envelope transition layers (the wind). ... Discovery of spectral variation in the optical counterpart of IRAS01005+7910. ... Dashed line - envelope curve of all the SiII 5979 profiles ...

... This matter may absorb the radiation from the source, scatter it or in fact emit fur ther radiation. ... For the case of a homogeneous cloud with a constant source function and optical depth with initial incident intensity , the emergent intensity is This makes a lot of sense: the emergent radiation is the sum of the incident intensity attenuated by the total optical depth plus the sum of each section of cloud emission attenuated by the optical ...

Stellarium 0.12.3 . ... Classes . ... FileљStructure . ... Atmosphere Class Reference . ... More... #include < Atmosphere.hpp > . voidљ . computeColor (double JD, Vec3d _sunPos, Vec3d moonPos, float moonPhase, StelCore *core, float eclipseFac, float latitude=45.f, float altitude=200.f, float temperature=15.f, float relativeHumidity=40.f) . ... Get fade in/out duration in seconds. ... getFlagShow () const . ... getFadeIntensity (void) const . ... Definition at line 40 of file Atmosphere.hpp . ...

... We present a computer program for modelling energy flux distribution and light curves of eclipsing binaries from far ultraviolet to infrared regions. The Roche model is assumed. Proximity effects of components (reflection of radiation and surface gravity darkening) are taken into account. ... Figure 1: The surface temperature distribution for Algol A-B system before (upper plot) and after (lower plot) correction for temperature due to the irradiation effect. ...

Wide-angle telescopes for photometry and polarimetry in optical and infrared ranges . ... Investigation of the Earth’s atmosphere, comets, interplanetary and interstellar medium with brightness and linear polarization measurements of extended sources and sky background in optical and infrared spectral ranges. ... The devices are small diameter telescopes with CCD-detectors for optical and infrared spectral range with spectral and polarization filters. ... 15-cm telescope with cooling down to 80 K . ...

The GSFC acousto-optic tunable filter (AOTF) camera was used at the Apache Point Observatory 3.5 meter telescope in Sunspot, NM, to image the night side of Venus. In the near-infrared, there are several spectral regions that are relatively clear in the Venus atmosphere. ... By imaging the Venus night side, an AOTF camera can determine spatial variations of trace molecular species in the Venusian atmosphere, and even study the dynamics of the zonal winds on Venus. ... APO Home Page . ...

... Design of Imaging Optics . Analyzing Optics . ... The high resolution near infrared camera (CONICA) for the first VLT unit telescope is under development. It serves as a multi-mode instrument for the wavelength region between 1.0 and 5.0 microns, providing diffraction-limited spatial resolution when combined with the adaptive optic system NAOS of the VLT (Rosset et al. ... VLT instrumentation, ALADDIN InSb detector, NIR imaging, NIR spectroscopy, re-imaging optics, IR optics . ...