![]() The 1980 eclipse of slide 9 occurred at the very peak of solar cycle 21 contrast the appearance of the white light corona then, with streamers appearing at all latitudes, with the solar minimum corona. It is roughly 3,000 to 5,000 kilometers (1,900 to 3,100 miles) in height, or slightly more than 1 of the Suns radius at maximum thickness, and possesses a homogeneous layer in the region directly above the photosphere. This layer marks the spot where the temperatures rise tremendously since the Corona layer is much hotter than the Chromosphere. Its width is only 60 miles, which is incredibly small for a layer on a body as large as the Sun. The corona is usually hidden by the bright light of the Sun’s surface. It is followed by the Transition region, which is an extremely narrow layer that divides the Chromosphere from the Corona. Note how the corona is reduced to a belt of streamers symmetrically straddling the solar equator. The Sun’s corona is the outermost part of the Sun’s atmosphere. The corona is the layer above these two layers. The bottom row shows a few eclipse photographs spanning the time period 1966–1988, together with a coronal image constructed from Solar Maximum Mission data for 1985, essentially at solar minimum. The photosphere has a thickness of about 500km, while the chromosphere is about 2,000km thick. The overall decrease in X-ray luminosity for the solar disk as a whole is in many ways as spectacular as the decrease in the number of active regions seen at a given time on the disk. It is almost certain that its energy comes from the Suns internal furnace, which also supplies the rest of the Suns heat. The top row of images are X-ray images from the Yohkoh satellite, spaced approximately 10 months apart during the descending part of cycle 22. Engulfed in the Suns brilliance, the corona reflects little visible sunlight and is barely visible to telescopes near Earth, a whopping 94 million miles (150 million kilometers) away. Soft X-ray images from the Yohkoh satellite. six or seven feet long, and of a uniform thickness of three-fourths of an inch. Not surprisingly, the changes in the surface magnetic field distribution through the solar cycle, as evidenced by the evolving numbers and spatial distributions of sunspots, prominences and filaments ( slide 17 and slide 18), are also reflected in the corona. nomena, writing about the suns corona, says: We must evidently wait.
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