Energy Telescope

The TOF energy telescope consists of two channel-plate timing detectors followed by a silicon energy detector. A simple short TOF spectrometer is also... 

The. experimental procedure was to use a BeO-B sample to adjust the total system such that the 10B4+ beam was maximized and the accelerator voltage was well-stabilized on the 9Be4+ beam. The mass -10 Faraday cup was then replaced by an energy-telescope preceded by a 16 mg/cm2 absorber, which prevented any 10B and other, higher-mass adventitious ions from over-loading the detectors. (Since the mass-10 cup is rotated into position in front of the detectors, the switch can be done easily, and it is possible to easily check the system periodically.) The irradiated BeO sample with 10Be/9Be ratio of 10 9 was arbitrarily selected as a standard and measurements of all other samples were made with respect to this standard. 

We propose a high energy telescope based on a CdTe PTF array in conjunction with a coded mask as an imaging spectrometer. In particular we suggest the construction of a 400 cm PSD using PTF CdTe crystals of 2x2 mm active area and 10 mm thickness. The detector wiU be surrounded by a BGO active shield ( 3 cm thick) and the detector FOV wiU be restricted to about 12°xl2° (FWHM) by means of a thin (400 fi) Tantalum tube coUimator efficient up to about 100 keV. 

Sputtered silver mirrors are used for solar energy (qv) collectors and astronomical telescope mirrors. Approximately 3 t/yr of silver are used in the United States for low emissivity windows. 

For ERDA arrangements using high-energy heavy projectiles, mainly gas telescope detectors, are used for AF and F measurements [3.153, 3.165, 3.166]. In an ionization... 

In 1994, a unique incident occurred the impact of the Shoemaker-Levy comet on the Jovian atmosphere. Die strong gravitational field of Jupiter caused the comet to break up before it could enter the atmosphere, and the parts of the comet crashed separately into the atmosphere one after the other. This unique spectacle was observed by many observatories and also by the Galileo spacecraft and the Hubble telescope. It led to the discovery of yet another phenomenon the most intensive aurora effects in the solar system, observed at Jupiter s poles. Astronomers assume that the energy for these comes from the planet s rotation, possibly with a contribution from the solar wind. This process differs from that of the origin of the aurora on Earth, where the phenomenon is caused by interactions between the solar wind and the Earth s magnetic field. 

To begin with, we must specify the spectral window we are referring to and then use the appropriate detector telescope, radiotelescope or space-borne observatory. The next characteristic is the accuracy of the energy, frequency or wavelength measurement, followed by the accuracy of the angular measurement (resolving power), and the temporal resolution and sensitivity of the measurement. Finally, we note the direction, date and duration of the observation for each particular celestial object we choose to investigate. 

As we cannot get hold of the stars, the galaxies and other universes, as we cannot manipulate them, we make models. In this way, numerical experiments provide support for telescopic observations, and for real experiments, such as those carried out in particle accelerators, which simulate energy conditions in the Big Bang and stars. 

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