Generally, researchers require observations from telescopes producing monochromatic images of coronal plasma images with cool, warm, and hot temperatures. To study solar activity, we need information about the plasma at different temperatures. Quiet Sun and active regions are at temperatures around 1 MK, while during flares, the coronal plasma can reach temperatures beyond 10 MK. Plasma in solar phenomena can be at a wide range of temperatures. A combination of the monochromatic Mg XII 8.42 Å, Si XIV 6.18 Å, and Si XIII 6.65 Å images will help us to study the dynamics of the hot plasma in the solar corona. In this article, we will review the design of the Mg XII spectroheliograph and present our thoughts on how to apply these principles to the Si XIV 6.18 Å and Si XIII 6.65 Å lines. We believe that these design principles can be applied to other spectral lines. Its design is based on two main principles: (1) to select the working wavelength and the crystal in such a way that reflection occurs at small incident angles (2) to use the aperture of the mirror as a spectral filter. The Mg XII spectroheliograph used Bragg crystal optics. Until now, monochromatic telescopic imaging has been made only in the Mg XII 8.42 Å line with the Mg XII spectroheliograph on board CORONAS-I, CORONAS-F, and CORONAS-PHOTON satellites. Generally, researchers require observations from telescopes producing monochromatic images of coronal plasma with cool, warm, and hot temperatures. Investigations of solar activity require information about plasma in a wide range of temperatures. Lebedev Physical Institute, Moscow, Russia Laboratory of the X-ray Astronomy of the Sun, P.N.The eclipse observations allow us to better understand this scattered light and improve calibrations of the instrument.Anton A. In fact, you do see a little bit of light and that is because of scattered light within the telescope. When the moon passes in front of the sun the detector on the X-ray telescope should go completely dark – you shouldn’t be able to see anything where the moon is. McCauley: The eclipse observation allows us to better calibrate the instruments aboard Hinode. Q: What can scientists learn by recording this solar eclipse? Instead, the center of the moon’s shadow was cast above Earth’s north pole, which allowed it to be viewed as an annular from Hinode’s perspective in orbit. McCauley: We could only see a partial eclipse because the Moon did not pass directly in front of the sun from our perspective on the ground. Q: Why couldn’t we see an annular eclipse from North America? That is hot enough to produce X-rays, which is what we are seeing with this telescope. The surface is about 5000 Kelvin and the corona can get up to 10 million Kelvin. The sun’s outer atmosphere is much hotter than its surface. The x-ray telescope on the Hinode satellite is used to monitor the outer atmosphere of the sun, called the corona. In this type of eclipse the moon’s shadow is not quite large enough to cover the full disc of the sun, resulting in a visible ring. An annular eclipse occurs when the moon passes directly between the observer and the sun. McCauley: We are looking at an annular eclipse that was observed by an X-ray telescope on the Hinode satellite. Q: What does the footage from the satellite show? While avid stargazers in North America looked up to watch the spectacle, the best vantage point was several hundred kilometers above the North Pole.Īstrophysicist Patrick McCauley from the Smithsonian’s Astrophysical Observatory explains how the Hinode satellite, which has a polar orbit, was in the perfect position to record a very different view of the solar eclipse. The moon passed between the Earth and the sun on Thursday, Oct.
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