![]() ![]() 2016, Vasquez et al., 2017, moving away from the Sun in its travel of near 100 AU or more until its encounter with the local interstellar medium (LISM, as it is explored in-situ, see e.g., Burlaga et al., 2013, Richardson et al., 2017, Cummings et al., 2016 ). ![]() It likely develops the slow solar wind (SW), see e.g. There are gaps, especially regarding a lack of understanding when it comes to the high temperature (more than 10 6 K) of the Sun Corona region starting possibly after the transition region (TR) above/near the chromosphere height, and up in altitude to a few solar radii, away from which it is understood that there begins the convection of matter and magnetic field. As well as the effects of radiative losses in the low corona and chromosphere, corona, transition region.” These statements, at least in part, sound true today. Additionally, some models ignore the effects of the inward flow of energy carried by thermal conduction from the hottest layers of the corona. When we consider the fundamental questions raised in Withbroe, 1988 : “The physical conditions in the Sun corona are vital to the development of an understanding of the mechanisms which heat the coronal plasma but exists uncertainty of these mechanisms. These results illustrate potential contribution to the understanding of the Sun corona, at least under specific conditions. 2018 showed how the COronal DEnsity and Temperature (CODET) model describes qualitative the K-corona over more than 11 years (solar cycles 23 and 24). On the other hand, earlier the work of Rodríguez Gómez et al. We propose a relatively simple schema for predicting the temperature and density of electrons in the solar corona, specifically in the “K-corona” (Berdichevsky et al. Where “ h” is a high with its origin measured vertically and away from an imaginary spherical surface defined by the photosphere surface. In the solar stratified atmosphere, the electron density (or gas pressure) falls off exponentially with height, while the temperature increases reaching more than 1 million K (Howard et al. They have been observed from the ground during eclipses and from space at distances as small as 0.3 astronomical units to the Sun. ) and the F-corona or zodiacal light which presents absorptionlines of the photospheric Fraunhofer spectrum caused by diffraction from interplanetary dust ( ) the L-corona consisting of spectral line emission from highly ionized atoms (at ![]() The solar corona observed in the white-light has three components: the K-corona, related to the solar photospheric light scattered by electrons (dominating at The Solar corona is the most external layer of the Sun. Non-dispersive acoustic speed is also expected to predict the observedĮquilibration time for the 1.1 to 1.3 R ⊙ quiescent corona during Perm eability properties and non-dispersive acoustic speed. Constitutive properties are derived from this novel state of nature, like magnetic With the CODET model prediction of a polytropic anomalous index for theĮlectron gas of the Sun’s corona. It is further noticed that this is wholly consistent Possesses a nature-state, non yet studied. It is shown that this magneto-matter has unusualĬharacteristics consistent with assuming that the low quiescent solar corona That medium is diamagnetic in the context of ideal The thermodynamic interpretationįinds consistency with the model of a magneto-matter medium possessing a 3-D Of hydro magnetism in global equilibrium. We reach a thermodynamic interpretation of the CODET model and itsĪccurate electron density and temperature prediction, grounded on the physics ![]()
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