Solar prominences with Na and Mg emissions and centrally reversed Balmer lines

Details Solar prominences with Na and Mg emissions and centrally reversed Balmer lines Solar prominences with Na and Mg emissions and centrally reversed Balmer lines

Mar 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005a%26a...431.1069s&link_type=abstract

Astronomy and Astrophysics, Volume 431, Issue 3, March I 2005, pp.1069-1073

Astronomy and Astrophysics

Astrophysics

4

Sun: Prominences, Radiation Mechanisms: Non-Thermal, Line: Formation

Scientific paper

We observed bright solar limb prominences with significant emission of NaD2 and Mgb2 simultaneously with the Hα, Hβ, HeD3, He^+4685, and the He^singl 5015 Å lines, using the THEMIS telescope on Tenerife. We find that most prominences with significant NaD2 and Mgb2 emissions show pronounced centrally reversed Hα profiles, and occasionally even of Hβ; the strongest emissions reach integrated intensities Eβ>16×{}104 [ erg/(cm2 s str)] . The centrally reversed profiles are well reproduced by semi-infinite models. The source function reaches Sα≤{}36 × {}104 [ erg/(cm2 s str Å)] corresponding to an excitation temperature T_exα≈3950 K; here, the optically thickness of Hα amounts τ^0α≈{}10. The line widths of the NaD2, Mgb2, and HeD3 profiles yield kinetic temperatures 7000≤{}T_kin<8000 K and non-thermal broadening v_tu=5 km s-1.

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