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1021. http://zebu.uoregon.edu/postscript/climate.ps
Climate Change: ffl Periodic Ice Ages: ! ... 100,000 years; \DeltaT 9 o F ffl Minor Period: ! 12,000 years; \DeltaT 5 o F ffl Smaller Periods ??: ! ... exposes con tinental shelfs ffl changes continental shelf composition due to in creased deposition during melt ffl changes hydrological cycle through less evapora tion ffl changes landscape ! ... Eastern Washington Causes of Ice Ages ffl needs to be PERIODIC! ffl Solar Cycle ! ... why periodic? ffl CO 2 Cycle ! ... 90,000 years ! ...
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Ссылки http://zebu.uoregon.edu/postscript/climate.ps -- 53.6 Кб -- 01.07.1994
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1022. http://zebu.uoregon.edu/postscript/atmos.ps
Evolution of Our Atmosphere Original Atmosphere of H/He Lost ffl Secondary Atmosphere liberated due to planetes imal collisions with protoearth that released volatiles trapped in grains ffl CO 2 + H 2 O (liquid) ) H 2 CO 3 (acid rain) ffl H 2 CO 3 + Ca ++ ) CaCO 3 (limestone) ffl H 2 CO 3 + CaMg(CO 3 ) 2 ) dolomites ffl N 2 ) chemically inert so it stays in atmosphere; N 2 cycle develops later ffl O 2 ) not present in original atmosphere; gotta make some critters first!
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Ссылки http://zebu.uoregon.edu/postscript/atmos.ps -- 44.4 Кб -- 01.07.1994
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1023. http://zebu.uoregon.edu/text/locos.txt
LOCOS = localized oxidation of silicon using silicon nitride as a mask against thermal oxidation.
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Ссылки http://zebu.uoregon.edu/text/locos.txt -- 1.1 Кб -- 01.06.1994
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1024. http://zebu.uoregon.edu/text/fs.txt
Frontside Illumination means the photons are indicident upon the electrode (gate) side of the CCD. Polysilicon layer has a typical thickness of 0.5 microns and hence photons with wavelength shorter than this (i.e. Blue Band) will interact with this layer producing an interference pattern. The preferential absorption of blue photons means low QE in the blue. ... In order for blue photons to reach the gates, however, the CCD must be thinned down a layer of about 10 microns in thickness. ...
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Ссылки http://zebu.uoregon.edu/text/fs.txt -- 1.7 Кб -- 01.06.1994
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1025. http://zebu.uoregon.edu/text/blabs.txt
W. Boyle and G. Smith, Charge Coupled Semiconductor Devices, Bell Systems Technical Journal, vol 49 pp. 587 --> April 1970
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Ссылки http://zebu.uoregon.edu/text/blabs.txt -- 1.1 Кб -- 01.06.1994
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1026. http://zebu.uoregon.edu/text/cte.txt
iCharge Transfer Efficiency is a measure of the percentage of electrons which are lost at each packet switching location. A 1000x1000 CCD would undergo 2000 such transfers upon readout. AT 98% CTE almost all the charge would be lost by the 2000th transfer. Consider a packet that contains 100,000 electrons, after 10 transfers there would be 18% packet loss and after 35 transfers there would be only 50% of the remaining charge and you still have another 1965 transfers to go!
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Ссылки http://zebu.uoregon.edu/text/cte.txt -- 1.5 Кб -- 31.05.1994
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1027. http://zebu.uoregon.edu/text/fss.txt
... These states can rapidly acquire charge as the potential well fills. ... The movement of electrons creates a drift component caused by the lateral electric field (this is a reflection of variations in the surface potential). ... This leads to two problems 1. if the voltage on gate one is reduce too slowly then the potential well under the gate retains charge 2. if reduced too quickly, majority carriers will return from the bulk to the surface and recombine causing a serious loss of charge. ...
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Ссылки http://zebu.uoregon.edu/text/fss.txt -- 1.9 Кб -- 31.05.1994
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1028. http://zebu.uoregon.edu/text/photoe.txt
Silicon exhibits an energy gap of 1.14 eV. Incoming photons with energy greater than this can excite valence electrons into the conduction band thus creating electron-hole pairs. ... Photons with energy of 1.1 to 5 eV generate single e-h pairs. ... Example: a 10 eV photon (Lyman alpha) will produce 3 e-h pairs, on average, for every incident photon. ... Limits in Silicon Detectors: Photons with energy less than 1.1 eV (about 1.2 microns) pass through silicon unimpeded. ...
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Ссылки http://zebu.uoregon.edu/text/photoe.txt -- 2.0 Кб -- 31.05.1994
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1029. http://zebu.uoregon.edu/messier/m13.txt
M3 and M13 two of the brightest globular clusters in the sky. Collectively, their light is equivalent to that of a 6th magnitude star. Their diameters are approximately 25 arcminutes so it can easily fill the field of view on many small telescopes.
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Ссылки http://zebu.uoregon.edu/messier/m13.txt -- 1.2 Кб -- 20.05.1994
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1030. http://zebu.uoregon.edu/messier/m100.txt
M100 is a challenging target. It has a diameter of 5.5 arcminutes and a total integrated magnitude of around 9.5. It is an excellent example of disk galaxy which has strong spiral structure. The Hubble pictures refer to only the inner 2.5x2.5 arcminutes of the galaxy, which corresponds to the brighter regions in the ground based blue CCD image.
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Ссылки http://zebu.uoregon.edu/messier/m100.txt -- 1.3 Кб -- 20.05.1994
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1031. http://zebu.uoregon.edu/messier/m17.txt
M17 is a gaseous nebula of ionized hydrogen, known as an H II region. It is very low in the southern summer sky for northern hemisphere observers and is a little less than 0.5 degrees in overall size. This image is an R-band (Red) image in which contains the principle emission lines of hydgrogen.
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Ссылки http://zebu.uoregon.edu/messier/m17.txt -- 1.3 Кб -- 20.05.1994
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1032. http://zebu.uoregon.edu/text/ionized.txt
Ionization is the process whereby an atom receives enough energy input (either via a collsion with another atom or by absorbing a photon) that the electron is stripped from the nucleus. That electron can later recombine with the nucleus and as it falls to the ground state, photons at discrete energies are emitted. These are called emission lines. Some of the images in these gallery are narrowband images that focus on the emission lines of oxygen as they are formed in this recombination process.
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Ссылки http://zebu.uoregon.edu/text/ionized.txt -- 1.5 Кб -- 19.05.1994
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1033. http://zebu.uoregon.edu/text/silva.txt
Ther eis nothing interesting here yet
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Ссылки http://zebu.uoregon.edu/text/silva.txt -- 1.0 Кб -- 05.05.1994
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1034. http://zebu.uoregon.edu/messier/m81.txt
M81 is one of the classic grand design spiral arm galaxies. ... Hubble Space Telescope OBSERvations have detected Cepheid Variables in the some fields on the outskirts of M81 and thus M81 is a fundamental calibrator of the Extragalactic Distance Scale. This exposure is taken through a blue filter using re-imaging optics on a 52-inch telescope. ... The exposure time was 30 seconds. ... The Ultraviolet Image of M81 comes from the Ultraviolet Imaging Telescope which is flown on the Shuttle. ...
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Ссылки http://zebu.uoregon.edu/messier/m81.txt -- 2.1 Кб -- 28.04.1994
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1035. http://zebu.uoregon.edu/messier/m57.txt
M57 is another famous and often photographed object. It is also known as the Ring Nebula. ... Of course, they have nothing to do with planets but rather represent late stages in the evolution of low mass stars in which a double shell source (Hydrogen and Helium Burning) around a non-fusing Carbon core is driving the outer layes of the star away, thus revealing a hotter star (the central star of the Planetary nebula). ... Here we present 3 images: 1. Normal black and white image 2. ...
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Ссылки http://zebu.uoregon.edu/messier/m57.txt -- 2.2 Кб -- 28.04.1994
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1036. http://zebu.uoregon.edu/messier/m101.txt
... It is extremely high surface brightness owing to star formation which is pervasive throughout the entire disk. Some very large H II regions can be found at large radii from its center, and this is somewhat unusual. The large number of massive stars now forming in M101 has made it an excellent case for study in the Ultraviolet, where faint extensions beyond the optical limit of the galaxy can be seen. ... This exposure was taken in the blue, again with reimaging optics on a 52-inch telescope. ...
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Ссылки http://zebu.uoregon.edu/messier/m101.txt -- 1.8 Кб -- 22.04.1994
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1037. http://zebu.uoregon.edu/messier/m95.txt
M95 is another example of a barred spiral. In fact, its overall appearance is quite similar to M91 except that M95 has more pronounced spiral structure. M95 is a good example of the kind of galaxy with a large range of intrinsic surface brightness. The large dynamic range of the CCD can capture all of this but the human eye or film will be dominated entirely by its bright center.
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Ссылки http://zebu.uoregon.edu/messier/m95.txt -- 1.4 Кб -- 22.04.1994
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1038. http://zebu.uoregon.edu/messier/m91.txt
This galaxy is rather small, about 5 x 5 arcminutes and is another difficult target for a small scope. It is a weakly barred galaxy with spiral arms emanating from the ends of the bar. The infrared CCD frame clearly shows the bar a little more clearly and shows the smooth spiral arms as outlined by an old stellar population.
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Ссылки http://zebu.uoregon.edu/messier/m91.txt -- 1.3 Кб -- 22.04.1994
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1039. http://zebu.uoregon.edu/messier/m90.txt
... M90 has an active nucleus. It is noteworthy in that M90 has a blueshift with respect to the Milky Way, even though it is located at a distance of 40 Million light years from us. This is because M90 is a member of the Virgo Cluster and its random velocity due to the gravitational potential well of Virgo is larger than its relative expansion velocity with respect to the Milky Way. That random component is accidentally pointed in our direction such that M90 has a velocity of about -250 km/s. ...
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Ссылки http://zebu.uoregon.edu/messier/m90.txt -- 1.7 Кб -- 22.04.1994
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1040. http://zebu.uoregon.edu/messier/m87.txt
This short exposure taken with the Kitt Peak 4-meter telescope clearly shows the large number of globular clusters that are associated with M87, the brightest elliptical galaxy in the Virgo cluster. The galaxy is also famous for having an active nucleus in which an outflow of collimated material is emanating. Note the very bright nucleus in the short exposure picture of M87 that helps to reveal the jet. M87 may mark the dynamical center of the Virgo cluster.
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Ссылки http://zebu.uoregon.edu/messier/m87.txt -- 1.5 Кб -- 22.04.1994
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