A Preliminary Report on the Magnetic Susceptibilities of by Hammar G.W.

By Hammar G.W.

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3. Filter magnetographs, equipped with a narrow-band birefringent filter as the spectroscopic analyzer and with a two-dimensional detector, trade spectral resolution for spatial extent. Filter magnetographs are used for detecting low magnetic flux densities and for following rapidly evolving features in the magnetic field – in these applications, pioneering work has been accomplished by means of the video magnetograph at Big Bear Solar Observatory. The magnetic calibration of filter magnetographs is less accurate than that of scanning spectrographic magnetographs.

Thermal conduction is negligible in stellar interiors except in very dense cores. If in a layer the energy flux L is carried by electromagnetic radiation alone, that layer is said to be in radiative equilibrium (RE). 1), and σ is the Stefan–Boltzmann constant. Often it is more convenient to use double-logarithmic temperature gradients defined by the following, and rewritten by means of Eqs. 9): ∇≡ d ln T H p dT R dT =− =− . ) The corresponding RE gradient is ∇RE = + 3κR ρ H p L . 2. 15) 14 Stellar structure where c p is the specific heat at constant pressure and cV is the specific heat at constant volume.

This fact is used in the improved Unno (1956) method developed by Robinson et al. 2. A simple two-component model, containing static magnetic and nonmagnetic components which do not radiatively interact, predicts V profiles that are strictly antisymmetric about the line center. However, the shape of many solar V profiles is different. , 1984; S´anchez Almeida and Lites, 1992). For comprehensive reviews of the observations and the interpretation of these departures of antisymmetry we refer to Solanki (1993, 1997).

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