Neutral atmospheric influences of the solar proton events in October–November 2003

Jackman, Charles H.; DeLand, Matthew T.; Labow, G. J.; Fleming, Eric L.; Weisenstein, Debra K.; Ko, Malcolm K. W.; Sinnhuber, Miriam; Russell, James M.

doi:10.1029/2004ja010888

Cited by 180 publications

(250 citation statements)

References 49 publications

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“…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: 97%

“…The ozone response due to very large SPEs is fairly rapid and substantial and has been observed during and after numerous events to date (e.g., Weeks et al, 1972;Heath et al, 1977;McPeters et al, 1981;Thomas et al, 1983;Solomon et al, 1982;McPeters and Jackman, 1985;Jackman et al, 1990Jackman et al, , 1995Jackman et al, , 2001Jackman et al, , 2005bJackman et al, , 2008Jackman et al, , 2011Jackman et al, , 2014 Decreases in mesospheric and upper stratospheric ozone are mostly caused by SPE-induced HO x increases, which were predicted to occur over 42 years ago (e.g., see Swider and Keneshea, 1973). Direct measurements of SPE-caused OH and HO 2 enhancements have confirmed these early predictions (e.g., Damiani et al, 2008;Jackman et al, 2011Jackman et al, , 2014).…”

Section: Solar Protonsmentioning

confidence: 99%

“…In the middle and upper mesosphere, one ion pair is computed to produce less than two HO x constituents per ion pair because water vapor decreases sharply with altitude there, and is no longer available as a source of HO x . For models which do not include D-region ion chemistry, we recommend using the parameterization of Solomon et al (1981), which is summarized following Jackman et al (2005b) in Table E1. If the partitioning between HO x species is considered in the model, H and OH should be formed in equal amounts.…”

Section: Appendix C: Recommendations For Geographic Projection Of Iprmentioning

confidence: 99%

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Solar forcing for CMIP6 (v3.2)

et al. 2017

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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...

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Section: Solar Protonsmentioning

confidence: 97%

Section: Solar Protonsmentioning

confidence: 99%

Section: Appendix C: Recommendations For Geographic Projection Of Iprmentioning

confidence: 99%

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Solar forcing for CMIP6 (v3.2)

et al. 2017

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“…As SEPs penetrate into the collisional atmosphere, they ionize neutrals along the way, greatly enhancing the electrical conductivity [Holzworth and Mozer, 1979;Holzworth et al, 1987]. Enhanced conductivity can cause communication disruptions (radio, GPS, avionics [Jones et al, 2005]) and can have significant impacts on atmospheric chemistry [Jackman et al, 2005;Verronen et al, 2005]. Under normal fair weather circumstances, the largest vertical electric fields in the atmosphere arise from the global electric circuit (GEC) [Wilson, 1920].…”

Section: Introductionmentioning

confidence: 99%

Rapid fluctuations of stratospheric electric field following a solar energetic particle event

Kokorowski

Sample

Holzworth

et al. 2006

Geophysical Research Letters

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During January, 2005, there were several large X‐class solar flares and associated solar energetic particle (SEP) events. Coincidentally, the MINIS balloon campaign had multiple payloads aloft in the stratosphere above Antarctica measuring dc electric fields, conductivity and x‐ray flux. One‐to‐one increases in the electrical conductivity and decreases to near zero of both the vertical and horizontal electric field components were observed in conjunction with an increase in particle flux at SEP onset. Combined with an atmospheric electric field mapping model, these data are consistent with a shorting out of the global electric circuit and point toward substantial ionospheric convection modifications. Additionally, two subsequent, rapid changes were detected in the vertical electric field component several hours after SEP onset. These changes result in similar fluctuations in the calculated vertical current density. We will describe how rigidity cut‐off dynamics may be crucial in understanding these sudden jumps in the vertical electric field.

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“…In the present work our scheme was updated to produce 1.25 odd nitrogen atoms per ion pair produced by cosmic rays, according to Jackman et al (1980), based on calculations of dissociation branching ratios from relativistic particle impact cross sections (Porter et al 1976). We introduced a parameterization whereby the GCR-induced N-production was split into two channels, i.e 45% ground-state N and 55% excited-state N (see Jackman et al 2005, and references therein). We also introduced an energydependence to the total N 2 ionization cross section by electron impact (Tabataba-Vakili et al 2016), replacing the constant electron impact cross section of 1.75 × 10 −16 cm 2 previously used with the energy-dependent cross section of Itikawa (2006).…”

Section: Cosmic-ray Schemementioning

confidence: 99%

Galactic cosmic rays on extrasolar Earth-like planets

Grießmeier

Vakili

Stadelmann

et al. 2016

A&A

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Context. Theoretical arguments indicate that close-in terrestial exoplanets may have weak magnetic fields. As described in the companion article (Paper I), a weak magnetic field results in a high flux of galactic cosmic rays to the top of the planetary atmosphere. Aims. We investigate effects that may result from a high flux of galactic cosmic rays both throughout the atmosphere and at the planetary surface. Methods. Using an air shower approach, we calculate how the atmospheric chemistry and temperature change under the influence of galactic cosmic rays for Earth-like (N 2 -O 2 dominated) atmospheres. We evaluate the production and destruction rate of atmospheric biosignature molecules. We derive planetary emission and transmission spectra to study the influence of galactic cosmic rays on biosignature detectability. We then calculate the resulting surface UV flux, the surface particle flux, and the associated equivalent biological dose rates. Results. We find that up to 20% of stratospheric ozone is destroyed by cosmic-ray protons. The effect on the planetary spectra, however, is negligible. The reduction of the planetary ozone layer leads to an increase in the weighted surface UV flux by two orders of magnitude under stellar UV flare conditions. The resulting biological effective dose rate is, however, too low to strongly affect surface life. We also examine the surface particle flux: For a planet with a terrestrial atmosphere (with a surface pressure of 1033 hPa), a reduction of the magnetic shielding efficiency can increase the biological radiation dose rate by a factor of two, which is non-critical for biological systems. For a planet with a weaker atmosphere (with a surface pressure of 97.8 hPa), the planetary magnetic field has a much stronger influence on the biological radiation dose, changing it by up to two orders of magnitude. Conclusions. For a planet with an Earth-like atmospheric pressure, weak or absent magnetospheric shielding against galactic cosmic rays has little effect on the planet. It has a modest effect on atmospheric ozone, a weak effect on the atmospheric spectra, and a noncritical effect on biological dose rates. For planets with a thin atmosphere, however, magnetospheric shielding controls the surface radiation dose and can prevent it from increasing to several hundred times the background level.

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Neutral atmospheric influences of the solar proton events in October–November 2003

Cited by 180 publications

References 49 publications

Solar forcing for CMIP6 (v3.2)

Solar forcing for CMIP6 (v3.2)

Rapid fluctuations of stratospheric electric field following a solar energetic particle event

Galactic cosmic rays on extrasolar Earth-like planets

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