By Magda Stavinschi (auth.), Jean-Paul Zahn, Magda Stavinschi (eds.)
The target of this complicated learn Institute was once to provide an account at the most up-to-date effects acquired in sunlight study. Bucharest was once selected to host it, as the capital urban of Romania used to be positioned correct in the midst of the totality direction of the final eclipse of the millennium, on eleventh August 1999; additionally the phenomenon was once with regards to succeed in there its longest period: 2m 23s. any such overall eclipse is not just a really staggering occasion which attracts the crowds: to astronomers, sun eclipses nonetheless supply the simplest stipulations for looking at the decrease a part of the corona. The sunlight performs an important position in our very life. It used to be chargeable for the formation of the Earth, and rendered this planet healthy to host dwelling beings, supplying the correct amount of warmth, and this for a protracted sufficient span of time. particularly understandably, it has continuously been a primary goal of human interest, and extra lately certainly one of medical research. over the last century, it was once discovered that the sunlight is a celeb like billions of others; we discovered when you consider that that it attracts its power from the nuclear fusion of hydrogen, and we're now capable of estimate its age and lifestyles expectancy.
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Extra 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
The cause of the structure difference between the observations in Ly-a and those in OVI could be due to: (a) A temperature effect: an electronic temperature higher in the emission region of OVI can affect the electrons population more than that involved in the emission of the neutral hydrogen; (b) A speed effect: the OVI lines are more sensitive to the Doppler effect than the In Ly-a line; (c) An abundance effect: if the oxygen is less abundant on the streamer axis than in the neighboring regions, its emission along the axis is diminished.
The Williams group on site was headed by Babcock, Kevin Russell, and Timothy McConnochie. Alexander Ene and Misa Cowee were in charge of an Ocean Optics spectrometer to monitor the central wavelength of the DayStar [Fe XIV] filter and Mark Kirby helped at the eclipse time. Previous work on this topic has been described by Pasachoff (1993) and Pasachoff et al. (1995a, 1995b). Phillips et al. (2000), after discussions with us, carried out a similar experiment. They used a higher cadence and a correspondingly lower statistical level of accuracy in the digitization, and the data should be complementary.
Studies of the heliosperic plasma could help to answer some questions about solar wind, such as: How do the properties of the SW evolve with distance from the Sun? How does the SW interact with the interstellar medium? What mechanisms are responsible for the SW accelerations? The large-scale coronal structure and phenomenology are very complicated by the solar magnetic field dynamics and its interaction with coronal plasma. There are coronal streamers, coronal mass ejections, coronal holes, and solar flares as proven contributors in the solar wind There are also polar plumes, the small-scale coronal phenomena, which could play a major role in the solar wind particle acceleration.