Advances in Solar Research at Eclipses from Ground and from by Magda Stavinschi (auth.), Jean-Paul Zahn, Magda Stavinschi

By Magda Stavinschi (auth.), Jean-Paul Zahn, Magda Stavinschi (eds.)

The target of this complex research Institute used to be to offer an account at the most up-to-date effects got in sunlight examine. Bucharest used to be selected to host it, as the capital urban of Romania used to be situated correct in the course of the totality direction of the final eclipse of the millennium, on eleventh August 1999; additionally the phenomenon was once with reference to succeed in there its longest length: 2m 23s. one of these overall eclipse isn't just a truly marvelous occasion which pulls the crowds: to astronomers, sunlight eclipses nonetheless provide the easiest stipulations for staring at the reduce a part of the corona. The solar performs an important position in our very life. It used to be liable for the formation of the Earth, and rendered this planet healthy to host dwelling beings, offering the correct amount of warmth, and this for an extended sufficient span of time. really understandably, it has constantly been a primary objective of human interest, and extra lately one in all medical research. over the last century, it was once discovered that the solar is a celeb like billions of others; we discovered for the reason that that it attracts its power from the nuclear fusion of hydrogen, and we're now capable of estimate its age and existence expectancy.

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Additional info for Advances in Solar Research at Eclipses from Ground and from Space: Proceedings of the NATO Advanced Study Institute on Advances in Solar Research at Eclipses from Ground and from Space Bucharest, Romania 9–20 August, 1999

Sample text

The first observations of the solar corona and its phenomena were obtained at total solar eclipses. Further eclipse observations could still be a good and necessary complement to the sophisticated space coronal observations. 2. Heliosphere Leverett Davis made the first suggestion about the existence and nature of the heliosphere in 1955 in connection with the cosmic rays dynamics. u. Figure 1. Schematic sketch of a plausible heliosphere generated by the flow of the solar wind and its interaction with the interstellar gas [7].

From the measurements made with UVCS certain physical parameters of the coronal streamers could be deduced, studying the widths of the spectral lines and the I3tion of the OVI doublets. Thus, for the kinetic temperature, the component along the line of sight in several spectral lines could be determined. 2x106 K at 5 RCi). There are no observation data on the velocity distribution (from which the kinetic tempemture can be obtained) perpendicular to the line of sight. 1032 lines. strongDoppleq)UlupiRg of the U037 line to great heights in the solar corona permits the determination of the upper limit of the kinetic tempemture of the OVI ions relative to the motions along the mdial direction.

From the measurements made with UVCS certain physical parameters of the coronal streamers could be deduced, studying the widths of the spectral lines and the I3tion of the OVI doublets. Thus, for the kinetic temperature, the component along the line of sight in several spectral lines could be determined. 2x106 K at 5 RCi). There are no observation data on the velocity distribution (from which the kinetic tempemture can be obtained) perpendicular to the line of sight. 1032 lines. strongDoppleq)UlupiRg of the U037 line to great heights in the solar corona permits the determination of the upper limit of the kinetic tempemture of the OVI ions relative to the motions along the mdial direction.

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