All stars derive their energy through the thermonuclear fusion of light elements in to heavy elements. High temperatures are required so that the mutual electrostatic repulsion of the protons in each fusing atomic nucleus is overcome. ... Elements with more protons in their nuclei require higher temperatures. ... This sequence is now shown in the animation below. ... First Step of the Proton-Proton Chain Narration . Second Step of the Proton-Proton Chain Narration . ...

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• Hydrogen as a Secondary Fuel
• Astronomy HyperText Book: Stellar Evolution

... High-pressures experiments are mostly aimed at studying phase transformations in solids, synthesising new phases and studying their composition, crystal and magnetic structure, physical and thermodynamical properties. ... The specific feature of investigations at LHPP that distinguishes it from most other high-pressure laboratories is combining in situ measurements with studies at ambient pressure of new high-pressure phases fixed by quenching to liquid nitrogen temperature. ...

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• Laboratory of Quantum Crystals
• Лаборатория квантовых кристаллов

... Orion Star Colours . ... Red stars are cool, around 3,000 kelvins (K), while blue stars are hotter and can have temperatures over 30,000 K. Our own lovely yellow Sun's temperature is a comforting 6,000 K. Hydrogen Trifid . ... Clouds of glowing hydrogen gas mingle with dark dust lanes in the Trifid Nebula, a star forming region in the constellation Sagittarius. ... These are galaxies of the Hercules Cluster, an archipelago of "island universes" a mere 650 million light-years distant. ... Vega . ...

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We present the detection and analysis of molecular hydrogen emission towards ten interstellar regions in the Large Magellanic Cloud. We examined low-resolution infrared spectral maps of 12 regions obtained with the Spitzer infrared spectrograph (IRS). ... The excitation diagrams of the detected H2 transitions are used to determine the warm H2 gas column density and temperature. ... We find the excitation of H2 by this process is equally efficient in both atomic- and molecular-dominated regions. ...

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• All kinds of death - 12
• ST ScI Preprint #1373
• Determining dust temperatures and masses in the Herschel era: The importance of

... Amorphous carbonaceous materials can show a great diversity of optical properties due to the variability in their microstructure. ... The differently pyrolized celluloses are representative for a suit of carbonaceous material ranging from strongly disordered (insulating) to graphitized (conducting) material. Figure: Complex refractive index of hydrogenated amorphous carbon prepared by pyrolysis (annealing) of cellulose at different temperatures. ...

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... The ionospheric plasma is composed of electrons and ions, freed from each other by ultraviolet energy from the sun. ... The spectrum below shows the widths associated with the hydrogen ions and the oxygen ions, assuming that they have the same temperatures. ... In the black and gray spectrum below, the oxygen ion and electron temperatures are the same. ... temperatures: electron, oxygen ion, and hydrogen ion . ion content: oxygen, helium, and hydrogen . velocities: oxygen ion and hydrogen ion. ...

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• ALFA Receiver Temperature Polynomial Fit
• dewarTemps
• Cold Hydrogen Clouds in the Milky Way: An Evolutionary Missing Link?

Get thermodynamics values for any combination of temperature, density and hydrogen mass fraction using MHD, OPAL or ISG equations of state. ... 3.0 < lg T < 7.5 . ... Hummer, D.G., Mihalas, D., 1988. Ap.J. 331 , 794-814. Mihalas, D., Dappen W. and Hummer, D.G., 1988. Ap.J., 331 , 815-825. Dappen, W., Mihalas, D., Hummer, D.G. and Mihalas, B.W., 1988. Ap.J., 332 , 261-270. ... Rogers, F.J., 1994. in IAU Colloq. ... Rogers, F.J., Swenson, F.J., Iglesias, C.A., 1996. ...

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... Since the reddening found for the stars in Table 13 was small, no reddening correction was attempted. ... These diamonds indicate the positions of very low mass, 3 Myr old, objects from the work of Burrows et al. ... This optical V versus R - I scheme is a very powerful method of detecting very low mass (VLM) objects. ... Because of this, young brown dwarfs are intrinsically no more difficult to observe in the optical than low mass stars at the age of Orionis. ...

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• Two-Temperature Raymond Model
• The AstroStat Slog temperature
• Cool Stars 10 - J.U. Drake and V. Kashyap: Coronal Metallicity of HR 1099

In this new series we present observations and modelling of spectral lines formed in main sequence star chromospheres (from G0 to M8). in this paper, we discuss the Hydrogen line formations in very active dMe stellar chromospheres. ... Our final model atmosphere is described in the next paper in this series. ... We found that observations are best reproduced by a chromospheric structure including a constant temperature gradient (in a log(M) scale) in the chromosphere and transition region. ...

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• The Sun | OASES Over us All is the SElfsame Sky | OASES 2010
• Armagh Observatory Preprint No. ???
• Adapted from "Why does the Sun Shine" | OASES Over us All is the SElfsame Sky |

... We computed the permanently shadowed areas and temperatures inside the craters for the variation of the position of the lunar pole of rotation with respect to the ecliptic pole with a period of 18.6 years. ... According to our results, the total permanently shadowed area in the polar craters of the Moon is equal to 50428.7 km2, or 0.13% of the total area of the lunar surface [3]. ... The area of permanently shaded part of a crater makes 59 % from all area of a crater [3]. ...

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• http://selena.sai.msu.ru/Symposium/RadioMoonE.doc
• http://selena.sai.msu.ru/Symposium/RadioMoonE.pdf
• http://selena.sai.msu.ru/Kozl/Publications/Houston2005(1).pdf

Next: Pressure Up: Additional information Previous: Additional information . ... Although the ESO Archive standard is to record temperatures in kelvins, this is often inconvenient. ... Therefore, if the temperatures are not in kelvins, the appropriate units should be provided in the table file (if temperatures are in a column), or as a comment. ... If filter and detector temperatures are otherwise regulated or recorded, it may still be useful to record DOMETEMP in the data file as a Real*4 column. ...

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• BTA meteo parameters: temperature for the last day
• BTA meteo parameters: temperature for the last year
• BTA meteo parameters: temperature for the last week

... Jupiter's Colorful Clouds . ... Explanation: What makes the colors in Jupiter's clouds ? With a mean temperature of 120 degrees Kelvin (-153 degrees Celsius) and a composition dominated by Hydrogen (about 90%), and Helium (about 10%) with a smattering of hydrogen compounds like methane and ammonia, astronomers have been hard pressed to explain the blue, orange and brown cloud bands and the salmon colored "red" spot. ... Alternatively, compounds of trace elements like sulfur may color the clouds. ...

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• APOD: September 20, 1997 - The Clouds of Jupiter
• APOD: 2013 July 31 - 130 Years of Earth Surface Temperatures
• APOD: January 30, 1997 - Earth's Temperature

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 . ...

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• Archive of ATNF Parkes Test Bed Archive Majordomo List
• Comptonization and Time-lags in Multi-Temperature Plasmas Surrounding Compact
• mmwave_mopra

. Next: Diameters Up: Stellar parameters from calibrations Previous: Gravities Contents . Temperatures of stars are derived from their spectral type and luminosity class. Calibrations are stored in files spec_par.V, spec_par.IV, spec_par.III, spec_par.II, spec_par.I in oyster/starbase . teff_stars Compute effective temperature for all stars in startable. teff_star ( spectrum _char ) Function. Return effective temperature for star with specified spectrum. Christian Hummel 2015-04-28

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• JupiterтАЩs Storms: Temperatures and Cloud Colours

Observational Stellar Astronomy . Articles | ... We are made of star stuff" . ... TEMPERATURE OF A STAR: . ... The temperature of a star can be found out easily by simple observations. ... STAR . ... SPECTRAL CLASS: . All the stars in this universe are divided in to spectral classes based on their spectral lines. ... The spectral class of a star and the temperature of a star are related. So the spectral class can be found for a star since we know its temperature. ... www.astronomy.net . ...

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... Gallery . Simulation Images . Simulations of convection in stars . Temperature contrast in part of a Solar simulтАж . Sidebar Left . Sidebar Top . No Sidebar . Sidebar Bottom . Sidebar Right . ... Title: Temperature contrast in part of a Solar simulation . ... NOTE: All images are copyright and must not be reproduced or mirrored in any form without written permission. ... Temperature contrast in part of a Solar simulation ?йRegner Trampedach . ...

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• Side-view of the temperatures in a simulation of a white dwarf
• Side-view of the temperatures in a simulation of the sub-giant Eta Bootes
• Emma Kirby - Science

Электронная библиотека астронома-любителя. ... библиотека . архив RSN . ... Ru.Space.News: . Ноябрь 2003 . ... I recently read an article that I found initially disturbing, but after reading the information on this site regarding the sun, I feel much more calm. ... A few people have requested more information about the temperature of the sun. The temperature at the center of the sun is about 16 million degrees Kelvin (27 million degrees Fahrenheit), as stated in the article. ...

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19. EMOS temperature check

20. Far-out Pathways to Space: Nuclear Power