Abstract
Abstract. The recent 23–30 January and 7–11 March 2012 solar proton event (SPE) periods were substantial and caused significant impacts on the middle atmosphere. These were the two largest SPE periods of solar cycle 24 so far. The highly energetic solar protons produced considerable ionization of the neutral atmosphere as well as HOx (H, OH, HO2) and NOx (N, NO, NO2). We compute a NOx production of 1.9 and 2.1 Gigamoles due to these SPE periods in January and March 2012, respectively, which places these SPE periods among the 12 largest in the past 50 yr. Aura Microwave Limb Sounder (MLS) observations of the peroxy radical, HO2, show significant enhancements of > 0.9 ppbv in the northern polar mesosphere as a result of these SPE periods. Both MLS measurements and Goddard Space Flight Center (GSFC) two-dimensional (2-D) model predictions indicated middle mesospheric ozone decreases of > 20% for several days in the northern polar region with maximum depletions > 60% over 1–2 days as a result of the HOx produced in both the January and March 2012 SPE periods. The SCISAT-1 Atmospheric Chemistry Experiment Fourier Transform Spectrometer (ACE) and the Envisat Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) instruments measured NO and NO2 (~ NOx), which indicated enhancements of over 20 ppbv in most of the northern polar mesosphere for several days as a result of these SPE periods. The GSFC 2-D model and the Global Modeling Initiative three-dimensional chemistry and transport model were used to predict the medium-term (~ months) influence and showed that the polar middle atmospheric ozone was most affected by these solar events in the Southern Hemisphere due to the increased downward motion in the fall and early winter. The downward transport moved the SPE-produced NOy to lower altitudes and led to predicted modest destruction of ozone (5–13%) in the upper stratosphere days to weeks after the March 2012 event. Polar total ozone reductions were predicted to be a maximum of 1.5% in 2012 due to these SPEs.
Highlights
Solar flares erupted in January and March 2012 and sent large fluxes of charged particles towards the Earth
The starting conditions for the two Goddard Space Flight Center (GSFC) 2-D model simulations used in this study were provided by a time dependent “spin-up” simulation from January 2000–December 2011, which included the appropriate source gas boundary conditions from WMO (2011) and the changing transport fields derived from Modern Era Retrospective-analysis for Research and Applications (MERRA) for this time period
The starting conditions for the two Global Modeling Initiative (GMI) 3-D chemistry and transport model (CTM) simulations used in this study were provided by a time dependent “spin-up” simulation from January 2004–December 2011, which included the appropriate source gas boundary conditions from WMO (2011) and the changing transport fields derived from MERRA for this time period
Summary
Solar flares erupted in January and March 2012 and sent large fluxes of charged particles towards the Earth. SPEs and their middle atmospheric constituent influences have been studied before (e.g., Swider and Keneshea, 1973; Heath et al, 1977; Solomon et al, 1981; McPeters and Jackman, 1985; Randall et al, 2001; López-Puertas et al, 2005a; von Clarmann et al, 2005; Verronen et al, 2006, 2008, 2011a, b; Krivolutsky et al, 2006; Funke et al, 2011; Jackman et al, 1990, 2001, 2005, 2007, 2008, 2009, 2011; Sinnhuber et al, 2012), each new event offers a chance to investigate the SPE-caused atmospheric perturbation under somewhat different conditions. The recent study of von Clarmann et al (2013) showed several atmospheric constituent changes due to the January and March 2012 SPEs using Envisat Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) instrument measurements These latest large events, which provided very significant middle atmospheric impulses over short (∼ days) periods of time, offer new opportunities to test the general understanding of an atmospheric change caused by very substantial perturbations.
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
