Line formation of He I D3 and He I 10830 Ã in a small-scale reconnection event

Abstract

Aims. We aim to explain line formation of He I D3 and He I 10830 Ã in small-scale reconnection events. Methods. We make use of a simulated Ellerman bomb (EB), present in a Bifrost-generated radiative Magnetohydrodynamics (rMHD) snapshot. The resulting He I D3 and He I 10830 Ã line intensities are synthesized in 3D using the non-LTE Multi3D code. We compare the synthetic helium spectra with observed SST/TRIPPEL raster scans of EBs in He I 10830 Ã and He I D3. Results. Emission in He I D3 and He I 10830 Ã is formed in a thin shell around the EB at a height of $\sim 0.8$ Mm while the He I D3 absorption is formed above the EB at $\sim 4$ Mm. The height at which the emission is formed corresponds to the lower boundary of the EB, where the temperature increases rapidly from $6\cdot 10^3$ K to $10^6$ K. The opacity in He I D3 and He I 10830 Ã is generated via photoionization-recombination driven by EUV radiation that is locally generated in the EB at temperatures in the range of $2\cdot 10^4-2\cdot 10^6$ K and electron densities between $10^{11}$ and $10^{13}$ cm${}^{-3}$. The synthetic emission signals are a result of coupling to local conditions in a thin shell around the EB, with temperatures between $7\cdot 10^3$ and $10^4$ K and electron densities ranging from $\sim 10^{12}$ to $10^{13}$ cm${}^{-3}$. Hence, both strong non-LTE as well as thermal processes play a role in the formation of He I D3 and He I 10830 Ã in the synthetic EB/UV burst that we studied. Conclusions. In conclusion, the synthetic He I D3 and He I 10830 Ã emission signatures are an indicator of temperatures of at least $2\cdot 10^4$ K and in this case as high as $\sim 10^6$ K.

12 pages, 13 figures, submitted to A&A