Hinode, TRACE, SOHO, and Ground-based Observations of a Quiescent Prominence

Details Hinode, TRACE, SOHO, and Ground-based Observations of a Quiescent Prominence Hinode, TRACE, SOHO, and Ground-based Observations of a Quiescent Prominence

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...686.1383h&link_type=abstract

The Astrophysical Journal, Volume 686, Issue 2, pp. 1383-1396.

Astronomy and Astrophysics

Astronomy

26

Sun: Prominences, Sun: Uv Radiation, Techniques: Spectroscopic

Scientific paper

A quiescent prominence was observed by several instruments on 2007 April 25. The temporal evolution was recorded in Hα by the Hinode SOT, in X-rays by the Hinode XRT, and in the 195 Å channel by TRACE. Moreover, ground-based observatories (GBOs) provided calibrated Hα intensities. Simultaneous extreme-UV (EUV) data were also taken by the Hinode EIS and SOHO SUMER and CDS instruments. Here we have selected the SOT Hα image taken at 13:19 UT, which nicely shows the prominence fine structure. We compare this image with cotemporaneous ones taken by the XRT and TRACE and show the intensity variations along several cuts parallel to the solar limb. EIS spectra were obtained about half an hour later. Dark prominence structure clearly seen in the TRACE and EIS 195 Å images is due to the prominence absorption in H I, He I, and He II resonance continua plus the coronal emissivity blocking due to the prominence void (cavity). The void clearly visible in the XRT images is entirely due to X-ray emissivity blocking. We use TRACE, EIS, and XRT data to estimate the amount of absorption and blocking. The Hα integrated intensities independently provide us with an estimate of the Hα opacity, which is related to the opacity of resonance continua as follows from the non-LTE radiative-transfer modeling. However, spatial averaging of the Hα and EUV data have quite different natures, which must be taken into account when evaluating the true opacities. We demonstrate this important effect here for the first time. Finally, based on this multiwavelength analysis, we discuss the determination of the column densities and the ionization degree of hydrogen in the prominence.

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