Spectral Diagnostics of the Magnetic Field Orientation in a Prominence Observed with SOHO/SUMER

Details Spectral Diagnostics of the Magnetic Field Orientation in a Prominence Observed with SOHO/SUMER Spectral Diagnostics of the Magnetic Field Orientation in a Prominence Observed with SOHO/SUMER

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007soph..241...53s&link_type=abstract

Solar Physics, Volume 241, Issue 1, pp.53-66

Physics

18

Prominences, Hydrogen Lyman Lines, Solar Magnetic Fields

Scientific paper

During several campaigns focused on prominences we have obtained coordinated spectral observations from the ground and from space. The SOHO/SUMER spectrometer allows us to observe, among others, the whole Lyman series of hydrogen, while the Hα line was observed by the MSDP spectrograph at the VTT. For the Lyman lines, non-LTE radiative-transfer computations have shown the importance of the optical thickness of the prominence corona transition region (PCTR) and its relation to the magnetic field orientation for the explanation of the observed line profiles. Moreover, Heinzel, Anzer, and Gunár (2005, Astron. Astrophys. 442, 331) developed a 2D magnetostatic model of prominence fine structures that demonstrates how the shapes of Lyman lines vary, depending on the orientation of the magnetic field with respect to the line of sight. To support this result observationally, we focus here on a round-shaped filament observed during three days as it was crossing the limb. The Lyman profiles observed on the limb are different from day to day. We interpret these differences as being due to the change of orientation of the prominence axis (and therefore the magnetic field direction) with respect to the line of sight. The Lyman lines are more reversed if the line of sight is across the prominence axis as compared to the case when it is aligned along its axis.

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