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This means that the coronal gas is a high-temperature plasma consisting of numerous free electrons and the ions of many kinds of atoms. Although hydrogen is completely ionized into free protons and electrons, other common elements such as oxygen, nitrogen and iron are not completely stripped of all their electrons. The corona is a dilute ‘upper atmosphere’ to the sun in which atoms become ionized at temperatures above 1 million Celsius. To understand these regions, we have to understand how matter and radiation interact.
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The E-corona is the weakest of the three within twice the sun’s radius and is generally not observable except by using a spectroscope, but more on that later. Even during a total solar eclipse, we see that the K-corona outshines the F an E coronas at distances closer than about twice the solar radius, but at greater distances it is the F-corona that completely dominates. Also is the brightness of the clear desert sky, and the sky during a total solar eclipse. The figure shows then brightness of the major K, F and E corona components in terms of their distance from the sun in units of the sun’s radius, and the intensity of the corona in terms of the brightness of the sun’s photosphere. To distinguish them they are called the K-corona, E-corona, F-corona, T-corona and the S-corona after ‘Kontinuierlich’ (Continuum), Emission, Fraunhofer, Thermal and Sublimation. But how does the corona shine? In fact, there isn’t simply one corona emitting light but five different solar corona, each produced by different light-emitting processes. Such surfaces emit electromagnetic radiation in the visible part of the spectrum near what the human eye and brain identify as the color yellow. We know that the sun shines because its surface has a temperature of 6000 Celsius. Eclipse: Who? What? When? Where? and How?.Additionally, any predicted CIR or CH HSS influences are explained in more detail in the forecast discussion. SWPC forecasters take into account any possible effects of CIR and CH HSS activity when forecasting the anticipated levels of overall planetary geomagnetic response for each 3-hour synoptic period over the next three days as detailed in the 3-day forecast. The larger and more expansive coronal holes can often be a source for high solar wind speeds that buffet Earth for many days.īecause of their potential for escalated geomagnetic activity and possible storming (G1 or higher), forecasters analyze coronal holes closely and also note them on the daily synoptic drawing. Geomagnetic storms are classified using a five-level NOAA Space Weather Scale. Strong CIRs and the faster CH HSS can impact Earth’s magnetosphere enough to cause periods of geomagnetic storming to the G1-G2 (Minor to Moderate) levels although rarer cases of stronger storming may also occur. Generally, coronal holes located at or near the solar equator are most likely to result in any CIR passage and/or higher solar wind speeds at Earth. After passage of the CIR and upon transition into the CH HSS flow, the overall IMF strength will normally begin to slowly weaken. As the CH HSS begins to arrive at Earth, solar wind speed and temperature increase, while particle density begins to decrease.
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The CIR can result in particle density enhancement and interplanetary magnetic field (IMF) strength increases preceding onset of the CH HSS. From the perspective of a fixed observer in interplanetary space, the CIR will be seen to lead the coronal hole high speed stream (CH HSS). As the high speed stream interacts with the relatively slower ambient solar wind, a compression region forms, known as a co-rotating interaction region (CIR). Persistent coronal holes are long-lasting sources for high speed solar wind streams. It is also possible for coronal holes to develop in isolation from the polar holes or for an extension of a polar hole to split off and become an isolated structure. Coronal holes are most prevalent and stable at the solar north and south poles but these polar holes can grow and expand to lower solar latitudes. The more persistent coronal holes can sometimes last through several solar rotations (27-day periods). This open, magnetic field line structure allows the solar wind to escape more readily into space, resulting in streams of relatively fast solar wind and is often referred to as a high speed stream in the context of analysis of structures in interplanetary space.Ĭoronal holes can develop at any time and location on the Sun, but are more common and persistent during the years around solar minimum. They appear dark because they are cooler, less dense regions than the surrounding plasma and are regions of open, unipolar magnetic fields. Coronal holes appear as dark areas in the solar corona in extreme ultraviolet (EUV) and soft x-ray solar images.