![]() Reliable profiles corrected for the input of the white-light corona and instrumental effects were selected for analysis of distributions of the line full width at half maximum (FWHM). Traces of faint emission is seen up to 1.8 R☉ for the 1981 corona. Eclipse “green” line (Fe XIV 5303 Å) Fabry-Perot interferograms obtained in 19 revealed fringes at distances of 1.1–1.5R☉. This allows to record line profiles at far distances. As a rule, totality sky brightness is significantly reduced resulting in imitation of space-borne conditions. Probably it also supplies silicon producing the IR-fluorescence corona from the SiO2 in the dust by the same mechanism.Įclipse line profiles of the E-corona (emission line corona) can provide direct data about velocity field in the range 2–4R☉ which seems to be the most interesting in sense of searching the regions of the solar wind acceleration. Dust corona supplies CO2 producing the fluorescent corona and CaO producing the sublima-tion corona by thermal decomposition of CaCO3 by its heating by hot plasma of the streamers of the electron corona. Large coronal streamers can be considered as a separate new component of the solar corona which may be called Fluorescent or Fl-corona. Such molecules and radicals can be produced by evaporation of the dust corona. They emit only in certain regions of the visible spectra as a resonance fluorescence of molecules and radicals due to their interaction with the solar wind and sunlight. We demonstrate that giant coronal streamers observed only from the orbital coronagraph LASCO and from stratospheric flights during total eclipses do not belong to the white corona. Ground images of the total solar eclipse on 29 March 2006 filtered by this technique exhibit the same main structures of the far solar corona as that recorded from the space up to 20 solar radii far from the Sun. Obtained images of the eclipsed solar corona are compared with the images from the Large Angle Space Coronagraph (LASCO)-C3 registered simultaneously from space. We used this new technique to study otherwise invisible details in the solar corona and to register the far solar corona far beyond previous ground observations. This method makes possible visualization of fine details of studied objects invisible for naked eye (due to the visually undetectably low differences of their brightness from the neighbor parts of the image). It allows research and estimation of the finest differences in the color and structure of the images. Here we develop a new technique for registration of the far solar corona from ground observa-tions. We consider those possible interactions of the solar plasma, which could produce such emission to explain observed phenomenon. We obtained several experimental evidences that the far coronal streamers (observed directly only from the space or stratosphere) do not emit or reflect white light, but emit only in in the visible light spectral regions. These speeds are so high that the particles can escape the Sun's gravity.Ĭonceptual animation (not to scale) showing the Sun's corona and solar wind.This work studies plasma interactions in the far solar corona. The corona's temperature causes its particles to move at very high speeds. From it comes the solar wind that travels through our solar system. We can view these features in detail with special telescopes. These include streamers, loops, and plumes. The Sun's magnetic fields affect charged particles in the corona to form beautiful features. This is the force that makes magnets stick to metal, like the door of your refrigerator. The surface of the Sun is covered in magnetic fields. But astronomers think that this is only one of many ways in which the corona is heated. In the corona, the heat bombs explode and release their energy as heat. The mission discovered packets of very hot material called "heat bombs" that travel from the Sun into the corona. Yet the corona is hundreds of times hotter than the Sun’s surface.Ī NASA mission called IRIS may have provided one possible answer. The corona is in the outer layer of the Sun’s atmosphere-far from its surface. This is the opposite of what seems to happen on the Sun.Īstronomers have been trying to solve this mystery for a long time. But when you walk away from the fire, you feel cooler. Imagine that you’re sitting next to a campfire. The corona’s high temperatures are a bit of a mystery. Image of corona from NASA's Solar Dynamics Observatory showing features created by magnetic fields. This low density makes the corona much less bright than the surface of the Sun. Why? The corona is about 10 million times less dense than the Sun’s surface. The corona reaches extremely high temperatures. Find tips on how to safely view an eclipse here. Remember to never look directly at the Sun, even during an eclipse.
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