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    Solar Images : sunImages 2009-03-31T11:24:02
    The Yohkoh satellite is an observatory for studying X-rays and gamma rays from the Sun. Launched from Kagoshima, Japan on August 31, 1991; Yohkoh is a project of the Institute for Space and Astronautical Sciences. The spacecraft was built in Japan and the observing instruments have contributions from the U.S. and from the U.K. ......
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    Geomagnetic And Solar Indices Data Description : geomInd 2009-03-31T11:24:02
    Geomagnetic indices constitute data series aiming at describing at a planetary scale the magnetic activity, or some of its components. The data series are homogeneous since 1932 for Kp and Ap, 1957 for Dst. ...
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    IMF and SWP Data Description : IMFMin : IMF 2009-03-31T11:24:02
    The interplanetary magnetic field (IMF) is a part of the Sun's magnetic field that is carried into interplanetary space by the solar wind. The interplanetary magnetic field lines are said to be "frozen in" to the solar wind plasma. Because of the Sun's rotation, the IMF, like the solar wind, travels outward in a spiral pattern that is often compared to the pattern of water sprayed from a rotating lawn sprinkler. The IMF originates in regions on the Sun where the magnetic field is "open"--that is, where field lines emerging from one region do not return to a conjugate region but extend virtually indefinitely into space. The direction (polarity, sense) of the field in the Sun's northern hemisphere is opposite that of the field in the southern hemisphere. (The polarities reverse with each solar cycle.)
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    Ionospheric Data : Iono 2009-03-31T11:24:01
    The ionosphere is that part of the upper atmosphere where free electrons occur in sufficient density to have an appreciable influence on the propagation of radio frequency electromagnetic waves. This ionization depends primarily on the Sun and its activity. Ionospheric structures and peak densities in the ionosphere vary greatly with time (sunspot cycle, seasonally, and diurnally), with geographical location (polar, auroral zones, mid-latitudes, and equatorial regions), and with certain solar-related ionospheric disturbances.
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    Geomagnetic Data : Intermag : Geom_yr : Geom_hr : Geom 2009-03-31T11:24:01
    To measure the Earth's magnetism in any place, we must measure the direction and intensity of the field. The parameters describing the direction of the magnetic field are declination (D), inclination (I). D and I are measured in units of degrees. The intensity of the total field (F) is described by the horizontal component (H), vertical component (Z), and the north (X) and east (Y) components of the horizontal intensity. These components may be measured in units of Oersted (1 oersted=1gauss) but are generally reported in nanoTesla (1nT * 100,000 = 1 0ersted). The Earth's magnetic field intensity is roughly between 25,000 - 65,000 nT (.25 - .65 oersted). Magnetic declination is the angle between magnetic north and true north. D is considered positive when the angle measured is east of true north and negative when west. Magnetic inclination is the angle between the horizontal plane and the total field vector.
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    Solar Data Description : SSN 2009-03-31T11:24:01
    The sun emits radio energy with a slowly varying intensity. This radio flux, which originates from atmospheric layers high in the sun's chromosphere and low in its corona, changes gradually from day-to-day, in response to the number of spot groups on the disk. Radio intensity levels consist of emission from three sources: from the undisturbed solar surface, from developing active regions, and from short-lived enhancements above the daily level. Solar flux density at 2800 megaHertz has been recorded routinely by radio telescope near Ottawa since February 14, 1947. Each day, levels are determined at local noon (1700 GMT) and then corrected to within a few percent for factors such as antenna gain, atmospheric absorption, bursts in progress, and background sky temperature. Beginning in June 1991, the solar flux density measurement source is Penticton, B.C., Canada.
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    NOAA GOES Satellite Mission : GOES 2009-03-31T11:24:01
    GOES satellites provide the kind of continuous monitoring necessary for intensive data analysis. They circle the Earth in a geosynchronous orbit, which means they orbit the equatorial plane of the Earth at a speed matching the Earth's rotation. This allows them to hover continuously over one position on the surface. The geosynchronous plane is about 35,800 km (22,300 miles) above the Earth, high enough to allow the satellites a full-disc view of the Earth. Because they stay above a fixed spot on the surface, they provide a constant vigil for the atmospheric "triggers" for severe weather conditions such as tornadoes, flash floods, hail storms, and hurricanes. When these conditions develop the GOES satellites are able to monitor storm development and track their movements.
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    Getting data 2009-03-31T11:21:32
    Getting data
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    SPIDR User Tutorial 2009-03-31T11:21:32
    SPIDR User Tutorial
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    SPIDR Datasets 2009-03-31T11:21:31
    This page is used to select the data categories and sets the user wants investigate in SPIDR.
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    Plotting data / Getting data / Using the data basket 2009-03-31T11:21:31
    Plotting data / Getting data / Using the data basket
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    Registration 2009-03-31T11:21:31
    Registration help
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    SPIDR Query 2009-03-31T11:21:31
    The "Detailed Data Set Request" page is used to select the date interval and time step for the SPIDR data set queries.
    rating: 0; views: 794; bookmark(s): 0; replies: 0       Bookmark