Stratospheric Ozone Variations Caused by Solar Proton Events Between 1963 and 2005

Jackman, Charles H.; Fleming, Eric L.

doi:10.1007/978-1-4020-6766-2_23

Cited by 2 publications

(5 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Although not statistically significant, we computed a modest ozone increase in the SH polar lower stratosphere (maximum >20%) as a result of the SPEs. This type of ozone behavior connected with large SPE‐induced NO y increases has been discussed before [ Jackman et al , 2000; Jackman and Fleming , 2008] and is related to the interference by NO y constituents with the halogen (chlorine and bromine) catalytic cycles (discussed further in section 4.2).…”

Section: Spe‐caused Long‐term Atmospheric Changes In Solar Cycle 23mentioning

confidence: 72%

“…A maximum polar ozone column decrease of about 1 to 4% due to very large SPEs has been computed in several previous two‐dimensional modeling studies [e.g., Jackman et al , 1990, 1995, 2000, 2005a, 2005b; Reid et al , 1991; Jackman and Fleming , 2008]. These earlier analyses were unable to reveal any SPE‐caused polar ozone column depletion in observations owing to the substantial intraseasonal and interannual variation in total ozone at high latitudes.…”

Section: Spe‐caused Long‐term Polar Atmospheric Changes In the 1963–2mentioning

confidence: 94%

“…The influence of very large SPEs in the first 9 years of solar cycle 23 (years 1996–2004) caused some significant documented changes in atmospheric composition, primarily during and within several months of the events [e.g., Randall et al , 2001; Jackman et al , 2001, 2005a, 2005b, 2008; Jackman and McPeters , 2004; Jackman and Fleming , 2008; Seppälä et al , 2004; Degenstein et al , 2005; López‐Puertas et al , 2005a, 2005b; Orsolini et al , 2005; von Clarmann et al , 2005; Rohen et al , 2005].…”

Section: Spe‐caused Long‐term Atmospheric Changes In Solar Cycle 23mentioning

confidence: 99%

“…Some modeling studies have addressed the longer‐term atmospheric influence of SPEs [e.g., Jackman et al , 1990, 1995, 2000, 2005a, 2005b; Reid et al , 1991; Semeniuk et al , 2005; Jackman and Fleming , 2008]. Only one of these previous studies [ Semeniuk et al , 2005] used a general circulation model (GCM).…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Long‐term middle atmospheric influence of very large solar proton events

et al. 2009

View full text Add to dashboard Cite

[1] The Whole Atmosphere Community Climate Model (WACCM3) has been used to study the long-term (more than a few months) effects of solar proton events (SPEs). Extremely large solar proton events occurred in 1972, 1989, 2000, 2001, and 2003 and caused some longer-lasting atmospheric changes. The highly energetic solar protons produced odd hydrogen (HO x ) and odd nitrogen (NO y ), which then led to ozone variations. Some statistically significant long-term effects on mesospheric ozone were caused by the HO x increases due to a very active time period for SPEs (years 2000-2004), even though the HO x increases were short-lived (days). The long-term stratospheric ozone effects were caused by the NO y enhancements. Very large NO y enhancements lasted for months in the middle and lower stratosphere after a few of the largest SPEs. SPE-caused NO y increases computed with WACCM3 were statistically significant at the 95% level throughout much of the polar stratosphere and mesosphere in the recent solar maximum 5-year period (2000)(2001)(2002)(2003)(2004). WACCM3-computed SPE-caused polar stratospheric ozone decreases of >10% continued for up to 5 months past the largest events; however, statistically significant ozone decreases were computed for only a relatively small fraction of this time in relatively limited altitudes in the lower mesosphere and upper stratosphere. Annually averaged model output showed statistically significant (to 95%) stratospheric ozone loss in the polar Northern Hemisphere for years [2000][2001][2002]. The computed annually averaged temperature and total ozone change in these years were not statistically significant.

show abstract

Section: Spe‐caused Long‐term Atmospheric Changes In Solar Cycle 23mentioning

confidence: 72%

Section: Spe‐caused Long‐term Polar Atmospheric Changes In the 1963–2mentioning

confidence: 94%

Section: Spe‐caused Long‐term Atmospheric Changes In Solar Cycle 23mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Long‐term middle atmospheric influence of very large solar proton events

et al. 2009

View full text Add to dashboard Cite

show abstract

“…The solar proton ionization rates are determined in the same way from GOES proton flux measurements as the daily ionization rates published by Jackman et al (), but with a higher time resolution. For an overview of the daily SPE ionization rate determination, see Jackman (). Ionization rates for energetic radiation belt electrons (30–1,000 keV) were implemented from the medium‐energy electron (MEE) model by van de Kamp et al ().…”

Section: Modelingmentioning

confidence: 99%

Cosmic Noise Absorption During Solar Proton Events in WACCM‐D and Riometer Observations

et al. 2019

View full text Add to dashboard Cite

Solar proton events (SPEs) cause large‐scale ionization in the middle atmosphere leading to ozone loss and changes in the energy budget of the middle atmosphere. The accurate implementation of SPEs and other particle ionization sources in climate models is necessary to understand the role of energetic particle precipitation in climate variability. We use riometer observations from 16 riometer stations and the Whole Atmosphere Community Climate Model with added D region ion chemistry (WACCM‐D) to study the spatial and temporal extent of cosmic noise absorption (CNA) during 62 SPEs from 2000 to 2005. We also present a correction method for the nonlinear response of observed CNA during intense absorption events. We find that WACCM‐D can reproduce the observed CNA well with some need for future improvement and testing of the used energetic particle precipitation forcing. The average absolute difference between the model and the observations is found to be less than 0.5 dB poleward of about 66° geomagnetic latitude, and increasing with decreasing latitude to about 1 dB equatorward of about 66° geomagnetic latitude. The differences are largest during twilight conditions where the modeled changes in CNA are more abrupt compared to observations. An overestimation of about 1° to 3° geomagnetic latitude in the extent of the CNA is observed due to the fixed proton cutoff latitude in the model. An unexplained underestimation of CNA by the model during sunlit conditions is observed at stations within the polar cap during 18 of the studied events.

show abstract

Stratospheric Ozone Variations Caused by Solar Proton Events Between 1963 and 2005

Cited by 2 publications

References 40 publications

Long‐term middle atmospheric influence of very large solar proton events

Long‐term middle atmospheric influence of very large solar proton events

Cosmic Noise Absorption During Solar Proton Events in WACCM‐D and Riometer Observations

Contact Info

Product

Resources

About