![]() By evaluating the magnetic energy of an elementary atom embedded in the magnetized medium obeying the macroscopic law B = μ 0( H + M), it is shown that the Zeeman Hamiltonian is due to the effect of H. They escape from lower layers in a quasi-static spreading, and accumulate in the photosphere. It is then assumed that electrons escape from the solar interior, where their thermal velocity is much higher than the escape velocity, in spite of the effect of protons. Their usual photospheric densities lead to very weak magnetization M, four orders of magnitude lower than H. ![]() Magnetization is due to plasma diamagnetism, which results from the spiral motion of free electrons or charges about the magnetic field. The objective of this paper is to explain these observations through the law B = μ 0( H + M) in magnetized media. This represents an inexplicable discrepancy with respect to the div B = 0 law.Īims. LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place Jules Janssen, 92195 Meudon, FranceĮ-mail: A recent review shows that observations performed with different telescopes, spectral lines, and interpretation methods all agree about a vertical magnetic field gradient in solar active regions on the order of 3 G km −1, when a horizontal magnetic field gradient of only 0.3 G km −1 is found. Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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