On the nature of prominence emission observed by SDO/AIA

TL;DR

This paper investigates the temperature sensitivity of SDO/AIA's 171 and 131 bands in observing solar prominences, revealing that emissions originate from plasma at temperatures above 4×10^5 K, thus providing insights into the prominence-corona transition region.

Contribution

It analyzes the emission-line contributions in AIA bands using synthetic spectra, clarifying the plasma temperature range detectable in prominence observations.

Findings

The 171 band is dominated by Fe IX emission, even without plasma above 10^6 K.

The 131 band is dominated by Fe VIII emission.

Prominence plasma at > 4×10^5 K is detectable by AIA.

Abstract

The Prominence-Corona Transition Region (PCTR) plays a key role in the thermal and pressure equilibrium of solar prominences. Our knowledge of this interface is limited and several major issues remain open, including the thermal structure and, in particular, the maximum temperature of the detectable plasma. The high signal-to-noise ratio of images obtained by the Atmospheric Imaging Assembly (AIA) on NASA's Solar Dynamics Observatory clearly show that prominences are often seen in emission in the 171 and 131 bands. We investigate the temperature sensitivity of these AIA bands for prominence observation, in order to infer the temperature content in an effort to explain the emission. Using the CHIANTI atomic database and previously determined prominence differential emission measure distributions, we build synthetic spectra to establish the main emission-line contributors in the AIA bands. We find that the Fe IX line always dominates the 171 band, even in the absence of plasma at > 10^6 K temperatures, while the 131 band is dominated by Fe VIII. We conclude that the PCTR has sufficient plasma emitting at > 4 10^5 K to be detected by AIA.