Lifetime and production rate of NO&amp;lt;sub&amp;gt;x&amp;lt;/sub&amp;gt; in the upper stratosphere and lower mesosphere in the polar spring/summer after the solar proton event in October–November 2003

Friederich, F.; Clarmann, T. von; Funke, B.; Nieder, Holger; Orphal, J.; Sinnhuber, Miriam; Stiller, G. P.; Wissing, Jan Maik

doi:10.5194/acpd-12-17703-2012

Cited by 7 publications

(11 citation statements)

References 21 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…SPE-caused NO x increases have been shown in several studies (e.g., McPeters, 1986;Zadorozhny et al, 1992Zadorozhny et al, , 1994Randall et al, 2001;López-Puertas et al, 2005a;Jackman et al, 1995Jackman et al, , 2005bJackman et al, , 2008Jackman et al, , 2011Jackman et al, , 2014Funke et al, 2011;Friederich et al, 2013). Other NO y constituents like HNO 3 , HNO 4 , N 2 O 5 , and ClONO 2 (e.g., López- Puertas et al, 2005b;Jackman et al, 2008;Funke et al, 2011;Damiani et al, 2012; as well as the total NO y family (e.g., Funke et al, 2011Funke et al, , 2014a have also been shown to increase as a result of large SPEs.…”

Section: Solar Protonsmentioning

confidence: 93%

“…The production of HO x relies on complicated ion chemistry that takes place after the initial formation of ion pairs (Swider and Keneshea, 1973;Frederick, 1976;Solomon et al, 1981;Sinnhuber et al, 2012). Solomon et al (1981) computed HO x production rates as a function of altitude and ion pair production rate.…”

Section: Appendix C: Recommendations For Geographic Projection Of Iprmentioning

confidence: 99%

See 1 more Smart Citation

Solar forcing for CMIP6 (v3.2)

et al. 2017

View full text Add to dashboard Cite

Abstract. This paper describes the recommended solar forcing dataset for CMIP6 and highlights changes with respect to CMIP5. The solar forcing is provided for radiative properties, namely total solar irradiance (TSI), solar spectral irradiance (SSI), and the F10.7 index as well as particle forcing, including geomagnetic indices Ap and Kp, and ionization rates to account for effects of solar protons, electrons, and galactic cosmic rays. This is the first time that a recommendation for solar-driven particle forcing has been provided for a CMIP exercise. The solar forcing datasets are provided at daily and monthly resolution separately for the CMIP6 preindustrial control, historical (1850CMIP6 preindustrial control, historical ( -2014, and future (2015-2300) simulations. For the preindustrial control simulation, both constant and time-varying solar forcing components are provided, with the latter including variability on 11-year and shorter timescales but no long-term changes. For the future, we provide a realistic scenario of what solar behavior could be, as well as an additional extreme Maunderminimum-like sensitivity scenario. This paper describes the forcing datasets and also provides detailed recommendations as to their implementation in current climate models.For the historical simulations, the TSI and SSI time series are defined as the average of two solar irradiance models that are adapted to CMIP6 needs: an empirical onePublished by Copernicus Publications on behalf of the European Geosciences Union. A new and lower TSI value is recommended: the contemporary solar-cycle average is now 1361.0 W m −2 . The slight negative trend in TSI over the three most recent solar cycles in the CMIP6 dataset leads to only a small global radiative forcing of −0.04 W m −2 . In the 200-400 nm wavelength range, which is important for ozone photochemistry, the CMIP6 solar forcing dataset shows a larger solar-cycle variability contribution to TSI than in CMIP5 (50 % compared to 35 %).We compare the climatic effects of the CMIP6 solar forcing dataset to its CMIP5 predecessor by using timeslice experiments of two chemistry-climate models and a reference radiative transfer model. The differences in the long-term mean SSI in the CMIP6 dataset, compared to CMIP5, impact on climatological stratospheric conditions (lower shortwave heating rates of −0.35 K day −1 at the stratopause), cooler stratospheric temperatures (−1.5 K in the upper stratosphere), lower ozone abundances in the lower stratosphere (−3 %), and higher ozone abundances (+1.5 % in the upper stratosphere and lower mesosphere). Between the maximum and minimum phases of the 11-year solar cycle, there is an increase in shortwave heating rates (+0.2 K day −1 at the stratopause), temperatures (∼ 1 K at the stratopause), and ozone (+2.5 % in the upper stratosphere) in the tropical upper stratosphere using the CMIP6 forcing dataset. This solar-cycle response is slightly larger, but not statistically significantly different from that for the CMIP5 forcing dataset.CMIP6 models wi...

show abstract

Section: Solar Protonsmentioning

confidence: 93%

Section: Appendix C: Recommendations For Geographic Projection Of Iprmentioning

confidence: 99%

Solar forcing for CMIP6 (v3.2)

et al. 2017

View full text Add to dashboard Cite

show abstract

“…This interaction makes it difficult to utilise regression or superposed epoch analysis in statistical studies of cosmic ray events. Reflecting this, atmospheric impacts of individual GLE events were analysed for 1989 (Mironova and Usoskin 2013(Mironova et al 2012), and 2000, 2001and 2003(Mironova and Usoskin 2014. The results suggested that an enhancement of ionisation rate by a factor of about 2 in the polar region with the night/cold/winter conditions can lead to formation or growing of aerosol particles in the polar middle stratosphere.…”

Section: Cosmic Raysmentioning

confidence: 99%

“…Verronen and Lehmann (2013) provided new parameterisation of ionic reactions affecting HO x and NO x production. Friederich et al (2013) calculated altitude-dependent NO x lifetimes and production rates from satellite observations. Several studies addressed the question of the role of transported NO x for the stratosphere.…”

Section: Energetic Particle Precipitationmentioning

confidence: 99%

What is the solar influence on climate? Overview of activities during CAWSES-II

Seppälä

Matthes

Randall

et al. 2014

Prog. in Earth and Planet. Sci.

View full text Add to dashboard Cite

This paper presents an overview of the main advances in the Key Questions identified by the Task Group 'What is the Solar Influence on Climate' by the SCOSTEP CAWSES-II science program. We go through different aspects of solar forcing from solar irradiance, including total solar irradiance (TSI) and solar spectral irradiance (SSI), to energetic particle forcing, including energetic particle precipitation (EPP) and cosmic rays (CR). Besides discussing the main advances in the timeframe 2009 to 2013, we also illustrate the proposed mechanism for climate variability for the different solar variability sources listed above. The key questions are as follows: What is the importance of spectral variations to solar influences on climate? What is the effect of energetic particle forcing on the whole atmosphere and what are the implications for climate? How well do models reproduce and predict solar irradiance and energetic particle influences on the atmosphere and climate?

show abstract

“…Ozone has a secondary peak in the mesospheric altitude and it significantly affects sodium concentration. The atmospheric ozone concentration undergoes depletion during solar proton event (SPE) as well established from modeling and observations [ Jackman et al , , , , , ; Seppälä et al , ; Degenstein et al , ; Rohen et al , ; Verronen et al , ; Krivolutsky et al , ; Friederich et al , ; Verkhoglyadova et al , , and references therein]. Krivolutsky et al [] and Jackman et al [] reported depletion in ozone concentration during SEPs in 23rd solar cycle using models.…”

Section: Introductionmentioning

confidence: 93%

Impact of M‐solar flare‐induced solar proton event on mesospheric Na layer over Utah (41.8°N,112°W)

Bag

2017

JGR Space Physics

View full text Add to dashboard Cite

The influence of solar proton event, induced by M‐solar flare, on the mesospheric sodium layer is studied over a midlatitude location Utah(41.8°N, 112°W) during 19 July 2012. The variation in sodium concentration (cm−3) is examined with temperature and atomic oxygen concentration obtained from NRLMSISE‐00 empirical model. In the vicinity of peak sodium concentration, the temperature shows a strong negative correlation with sodium concentration, atomic oxygen concentration shows a positive correlation with sodium concentration. An enhancement in sodium concentration is observed during the solar proton event with highest concentration at the time of maximum proton flux. The altitude of peak sodium concentration shows a downward movement with lowest altitude corresponding to the time of maximum proton flux. However, the altitude of peak sodium concentration is found in the altitude region of 85–90 km throughout the solar proton event.

show abstract

Lifetime and production rate of NO<sub>x</sub> in the upper stratosphere and lower mesosphere in the polar spring/summer after the solar proton event in October–November 2003

Cited by 7 publications

References 21 publications

Solar forcing for CMIP6 (v3.2)

Solar forcing for CMIP6 (v3.2)

What is the solar influence on climate? Overview of activities during CAWSES-II

Impact of M‐solar flare‐induced solar proton event on mesospheric Na layer over Utah (41.8°N,112°W)

Contact Info

Product

Resources

About