Preferred systems employ a focusing mirror as a primary concentrative device and a non-imaging concentrator as a secondary concentrative device with concentrative capacities of primary and secondary stages selected to provide for net solar flux intensification of greater than 2000 over 95 percent of the concentration area. O'Gallagher, Joseph J.ĭisclosed are multi-stage systems for high flux transformation of solar energy allowing for uniform solar intensification by a factor of 60,000 suns or more. Finally, we illustrate how 304 â„« images can be used as a proxy for magnetic flux measurements when magnetic field data is not accessible.« less To investigate this magnetic flux decay over several rotations we use a surface flux transport model, the Advective Flux Transport model, that simulates convective flows using a time- varying velocity field and find that the model provides realistic predictions when information about the active region's magnetic field strength and distribution at peak flux is available. Since STEREO does not make direct observations of the magnetic field, we employ a flux-luminosity relationship to infermore » the total unsigned magnetic flux evolution. We find that active regions typically follow a standard pattern of emergence over several days followed by a slower decay that is proportional in time to the peak intensity in the region. We use He ii 304 â„« data from these observatories to isolate and track ten active regions and study their long-term evolution. With multiple vantage points around the Sun, Solar Terrestrial Relations Observatory (STEREO) and Solar Dynamics Observatory imaging observations provide a unique opportunity to view the solar surface continuously. Ugarte-Urra, Ignacio Upton, Lisa Warren, Harry P. MAGNETIC FLUX TRANSPORT AND THE LONG-TERM EVOLUTION OF SOLAR ACTIVE REGIONS The major destruction channel for OH is predissociation, while direct photodissociation and solar wind interactions account for roughly 30 and 10 percent of the destruction rate, respectively. The calculated H2O and OH lifetimes against direct photodissociation both vary by 30 percent with solar activity. It is calculated that photodissociation accounts for about 80 percent of the H2O destruction rate, while photoionization and solar wind particle interactions each account for about 10 percent of the H2O destruction. It is shown that both the fluxes and variabilities of the model are more consistent with SME and SUSIM solar spectrum measurements than those of the SERF1 model. D.Ī solar EUV/FUV flux model based on recent SUSIM solar observations is presented. Solar flux variability and the lifetimes of cometary H2O and OHīudzien, S. High- Flux Solar Furnace Facility High- Flux Solar Furnace Facility NREL's High- Flux Solar Furnace (HFSF) is a 10-kW optical furnace for testing high-temperature processes or applications requiring high range of technologies with a diverse set of experimental requirements. High- Flux Solar Furnace Facility | Concentrating Solar Power | NREL Applications include study of solar energy and transfer of heat, and space power/ solar-dynamics engineering. Results compare favorably with those of more complicated programs. Simplified Calculation of Solar Flux Distribution on Side Wall of Cylindrical Cavity Solar Receivers computer program employs simple solar-flux-calculation algorithm for cylindrical-cavity-type solar receiver. Simplified Calculation Of Solar Fluxes In Solar Receivers Through this analysis, it was found that the power intensities of solar flux index show a high spectral variability. We also observed periodicities on solar flux index using wavelet analysis. Results also show that solar intensities higher during the rising phase of solar cycle. We also observed the solar cycle dependence on solar flux index and found a strong dependence on solar activity. We also analyzed the dataset obatained from riometer.Both instruments show seasonal and yearly variations. Both seasonal and yearly variation on solar F10.7 index. This study mainly focused on the variation on solar flux index and amount of electromagnetic wave in the atmosphere. The solar flux index is more often used for the prediction and monitoring of the solar activity. A 10.7 cm solar flux measurement is a determination of the strength of solar radio emission. During the time period of solar activity sunspots number will vary. Sometimes the greatest event occurs in the period of solar maxima and the lowest activity occurs in the period of solar minimum. Solar activities change within the period of 11 years. Periodicities observed on solar flux index (F10.7) during geomagnetic disturbancesĪdhikari, B.
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