Effects of Energetic Particles on Minor Constituents of the Middle Atmosphere

Jackman, Charles H.

doi:10.5636/jgg.43.supplement2_637

Cited by 23 publications

(10 citation statements)

References 44 publications

(55 reference statements)

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“…Volcanoes in years 1963, 1982, and 1991 caused large increases in the aerosol surface area. Enhanced aerosol surface area results in an increase in heterogeneous reactions on the sulfate aerosols.…”

Section: Aerosol Surface Areamentioning

confidence: 99%

“…The influence of GCRs on the middle atmosphere has been studied since the 1970s (e.g., Warneck, 1972;Ruderman and Chamberlain, 1975;Nicolet, 1975;Jackman et al, 1980Jackman et al, , 1987Jackman et al, , 1996Thorne, 1980;Garcia et al, 1984;Legrand et al, 1989;Jackman, 1991Jackman, , 1993Müller and Crutzen, 1993;Vitt and Jackman, 1996;Krivolutsky et al, 1999Krivolutsky et al, , 2001Krivolutsky et al, , 2002Vitt et al, 2000;Semeniuk et al, 2011;Calisto et al, 2011). These previous studies made use of GCR-produced ionization rates (GPIR) in computing atmospheric chemistry impacts.…”

Section: Introductionmentioning

confidence: 99%

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Atmospheric changes caused by galactic cosmic rays over the period 1960–2010

et al. 2016

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Abstract. The Specified Dynamics version of the Whole Atmosphere Community Climate Model (SD-WACCM) and the Goddard Space Flight Center two-dimensional (GSFC 2-D) models are used to investigate the effect of galactic cosmic rays (GCRs) on the atmosphere over the 1960-2010 time period. The Nowcast of Atmospheric Ionizing Radiation for Aviation Safety (NAIRAS) computation of the GCRcaused ionization rates are used in these simulations. GCRcaused maximum NO x increases of 4-15 % are computed in the Southern polar troposphere with associated ozone increases of 1-2 %. NO x increases of ∼ 1-6 % are calculated for the lower stratosphere with associated ozone decreases of 0.2-1 %. The primary impact of GCRs on ozone was due to their production of NO x . The impact of GCRs varies with the atmospheric chlorine loading, sulfate aerosol loading, and solar cycle variation. Because of the interference between the NO x and ClO x ozone loss cycles (e.g., the ClO + NO 2 + M → ClONO 2 + M reaction) and the change in the importance of ClO x in the ozone budget, GCRs cause larger atmospheric impacts with less chlorine loading. GCRs also cause larger atmospheric impacts with less sulfate aerosol loading and for years closer to solar minimum. GCR-caused decreases of annual average global total ozone (AAGTO) were computed to be 0.2 % or less with GCR-caused column ozone increases between 1000 and 100 hPa of 0.08 % or less and GCR-caused column ozone decreases between 100 and 1 hPa of 0.23 % or less. Although these computed ozone impacts are small, GCRs provide a natural influence on ozone and need to be quantified over long time periods. This result serves as a lower limit because of the use of the ionization model NAIRAS/HZETRN which underestimates the ion production by neglecting electromagnetic and muon branches of the cosmic ray induced cascade. This will be corrected in future works.

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Section: Aerosol Surface Areamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Atmospheric changes caused by galactic cosmic rays over the period 1960–2010

et al. 2016

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“…The 130 chemical reac-tions used are specified in the JPL 90-1 model (De More, 1990) with ground boundary conditions for the trace gases taken from WMO (1992). The residual circulation and diffusion specification is the Dynamics A formulation described in Jackman (1991). The maximum OH enhancement and associated 03 decrease that would result from such an electron flux if it were assumed to be constant for five hours is shown in Fig.…”

Section: Model Description and Resultsmentioning

confidence: 99%

Mesospheric Heating during Highly Relativistic Electron Precipitation Events.

Goldberg

Baker

Herrero

et al. 1995

J. geomagn. geoelec

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Highly relativistic electron precipitation (HRE) events which occur in the mid-latitude and auroral regions last 2.5 days on the average, peaking in the magnetosphere daily near local noon. Furthermore, they can recur every 27 days for several synodic solar rotation periods, and become most intense and frequent during the minimum of the solar cycle. These events are described in terms of their spatial and temporal extent and their spectral characteristics. A detailed sounding rocket study of a relatively weak event in May, 1990 at Poker Flat, Alaska gave energy depositions from which modeling calculations have yielded 03 depletion estimates in excess of 25% near 75 km altitude. These depletions would hardly affect the UV flux reaching the stratosphere below, but could alter the thermal balance in the 60-75 km altitude region in the mesosphere. Further analysis for that HRE has shown the possibility of Joule heating effects near the polar cusp of up to 3°/day depending on the magnitude of the electric field. The mesospheric heating caused by more intense events studied with SAMPEX (Solar Anomalous Magnetospheric Particle Explorer) is compared with the earlier May 1990 event to demonstrate the global impact of HRE events on the chemical and thermal characteristics of the neutral atmosphere.

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“…One effect of the ionization at middle atmosphere altitudes is an increased production rate of odd nitrogen and odd hydrogen compounds which play a significant role in the chemistry of middle atmosphere, including the ozone chemistry (Jackman, 1991). For example, at an altitude of 50 km, the electron spectrum of Figure 4 and the bremsstrahlung x-rays produced by them would enhance the production rate of odd nitrogen by a factor of [0-100 over cosmic ray background levels.…”

Section: Discussionmentioning

confidence: 99%

Observations of the UARS Particle Environment Monitor and computation of ionization rates in the middle and upper atmosphere during a geomagnetic storm

Sharber¹,

Frahm²,

Winningham³

et al. 1993

Geophysical Research Letters

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During the geomagnetic storm of 8–9 November 1991, the Upper Atmosphere Research Satellite (UARS), orbiting at 585 km, passed through the expanded auroral zone during portions of several successive orbits. The instruments of the UARS Particle Environment Monitor (PEM) observed particle precipitation, auroral x‐ray emissions, and large‐scale disturbances in the geomagnetic field during this time. In this paper we present observations made by the PEM instruments during this storm and compute ionization and energy deposition rates as functions of altitude in the middle and upper atmosphere by incident electrons and positive ions in the storm interval. The suite of PEM instruments provides a systematic measurement of energetic particles and their associated x‐rays over an energy range not fully covered by previous satellite missions. In this energy range the ionization and dissociation rate in the atmosphere may be inferred from the upper stratosphere to the thermosphere. The impact on the chemistry of the region may be investigated.

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Effects of Energetic Particles on Minor Constituents of the Middle Atmosphere

Cited by 23 publications

References 44 publications

Atmospheric changes caused by galactic cosmic rays over the period 1960–2010

Atmospheric changes caused by galactic cosmic rays over the period 1960–2010

Mesospheric Heating during Highly Relativistic Electron Precipitation Events.

Observations of the UARS Particle Environment Monitor and computation of ionization rates in the middle and upper atmosphere during a geomagnetic storm

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