15 years of VLT/UVES OH intensities and temperatures in comparison with TIMED/SABER data. (October 2017)

• Record Type: Journal Article
• Authors: Noll, Stefan; Kimeswenger, Stefan; Proxauf, Bastian; Unterguggenberger, Stefanie; Kausch, Wolfgang; Jones, Amy M.
• Is Part Of: Journal of atmospheric and solar-terrestrial physics. Volume 163(2017)
• Page Start: 54
• Page End: 69
• Publication Date: 2017-10
• Subjects: OH emission -- Spectroscopy -- Temperature -- Solar cycle; Geophysics -- Periodicals; Atmospheric physics -- Periodicals; Géophysique -- Périodiques; Météorologie physique -- Périodiques; Electronic journals; 551.51
• DOI: 10.1016/j.jastp.2017.05.012
• Languages: English
• ISSNs: 1364-6826

Abstract

Abstract: The high-resolution echelle spectrograph UVES of the Very Large Telescope at Cerro Paranal in Chile has been regularly operated since April 2000. Thus, UVES archival data originally taken for astronomical projects but also including sky emission can be used to study airglow variations on a time scale longer than a solar cycle. Focusing on OH emission and observations until March 2015, we considered about 3000 high-quality spectra from two instrumental set-ups centred on 760 and 860 nm, which cover about 380 nm each. These data allowed us to measure line intensities for several OH bands in order to derive band intensities and rotational temperatures for different upper vibrational levels as a function of solar activity and observing date. The results were compared with those derived from emission and temperature profile data of the radiometer SABER on the TIMED satellite taken in the Cerro Paranal area between 2002 and 2015. In agreement with the SABER data, the long-term variations in OH intensity and temperature derived from the UVES data are dominated by the solar cycle, whereas secular trends appear to be negligible. Combining the UVES and SABER results, the solar cycle effects for the OH intensity and temperature are about 12–17% and 4–5 K per 100 sfu and do not significantly depend on the selected OH band. The data also reveal that variations of the effective OH emission layer height and air density can cause significant changes in the OH rotational temperatures due to a varying ratio of OH thermalising collisions by air molecules and OH radiation, deactivation, and destruction processes which impede the rotational relaxation. However, this effect appears to be of minor importance for the explanation of the rotational temperature variations related to the solar activity cycle, which causes only small changes in the OH emission profile. Highlights: High-resolution VLT/UVES spectra of multiple OH bands taken between 2000 and 2015. OH intensities and rotational temperatures show strong solar cycle effects. Good agreement with SABER OH data taken close to the VLT between 2002 and 2015. No significant long-term trend in UVES and SABER OH intensities and temperatures. Weak non-LTE contributions to long-term variations in OH rotational temperatures.