Modeling of Hα Eruptive Events Observed at the Solar Limb

• Published in: Solar physics Vol. 284; no. 2; pp. 447 - 466
• Main Authors: Kotrč, P., Bárta, M., Schwartz, P., Kupryakov, Y. A., Kashapova, L. K., Karlický, M.
• Format: Journal Article
• Language: English
• Published: Dordrecht Springer Netherlands 01-06-2013
• Subjects: Advances in European Solar Physics; Astrophysics and Astroparticles; Atmospheric Sciences; Physics; Physics and Astronomy; Space Exploration and Astronautics; Space Sciences (including Extraterrestrial Physics; Chromosphere; Eruptions; Flares; MHD; Models; Radio flux; Spectrum
• ISSN: 0038-0938; 1573-093X
• DOI: 10.1007/s11207-012-0167-6

We present spectra and slit-jaw images of limb and on-disk eruptive events observed with a high temporal resolution by the Ondřejov Observatory optical spectrograph. Analysis of the time series of full width at half-maximum (FWHM) in Hα, Hβ, and radio and soft X-ray (SXR) fluxes indicates two phenomenologically distinct types of observations which differ significantly in the timing of FWHM and SXR/radio fluxes. We investigated one such unusual case of a limb eruptive event in more detail. Synthesis of all observed data supports the interpretation of the Hα broadening in the sense of regular macroscopic plasma motions, contrary to the traditional view (emission from warm dense plasma). The timing and observed characteristics indicate that we may have actually observed the initiation of a prominence eruption. We test this scenario via modeling of the initial phase of the flux rope eruption in a magnetohydrodynamic (MHD) simulation, calculating subsequently – under some simplifying assumptions – the modeled Hα emission and spectrum. The modeled and observed data correspond well. Nevertheless, the following question arises: To what extent is the resulting emission sensitive to the underlying model of plasma dynamics? To address this issue, we have computed a grid of kinematic models with various arbitrary plasma flow patterns and then calculated their resulting emission. Finally, we suggest a diagnostics based on the model and demonstrate that it can be used to estimate the Alfvén velocity and plasma beta in the prominence, which are otherwise hard to obtain.