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Evidence against turbulent and canopy-like magnetic fields in the solar chromosphere


Measurements of the degree of polarization of light in the spectral lines emitted by gas near the Sun's limb (its outer edge) can be used to investigate the electron densities and magnetic field strengths in the solar atmosphere; these quantities are important for determining the balance and transport of energy through the Sun's atmosphere. Recent measurements1,2 revealed a surprising degree of polarization in the sodium doublet; these observations have remained an enigma. Here I report a mechanism that may explain these observations, in which it is assumed that the populations of the magnetic sublevels of the electronic ground state of the sodium atom are not equal: this leads to ground-level atomic polarization. This mechanism explains very well the observed line shapes, and implies that depolarization does not occur in the solar chromosphere, which would seem to rule out the existence of turbulent magnetic fields and of horizontal, canopy-like fields stronger than0.01 G. This is difficult to understand, because there is substantial evidence from othertypes of observation for both types of field3,4,5,6,7,8,9,10. There are obviously aspects of the Sun's atmosphere that remain very poorly understood.

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Figure 1: Polarization profiles Q/I, with the positive Q-direction defined as the tangent to the solar limb.


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I thank J. O. Stenflo for helping in the presentation of the Letter and for providing the original data shown in Fig. 1.

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Correspondence to Egidio Landi Degl'Innocenti.

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Degl'Innocenti, E. Evidence against turbulent and canopy-like magnetic fields in the solar chromosphere. Nature 392, 256–258 (1998).

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