Journal topic
Atmos. Chem. Phys., 18, 11905–11925, 2018
https://doi.org/10.5194/acp-18-11905-2018
Atmos. Chem. Phys., 18, 11905–11925, 2018
https://doi.org/10.5194/acp-18-11905-2018

Research article 21 Aug 2018

Research article | 21 Aug 2018

# Changes in clouds and thermodynamics under solar geoengineering and implications for required solar reduction

Changes in clouds and thermodynamics under solar geoengineering and implications for required solar reduction
Rick D. Russotto1 and Thomas P. Ackerman1,2 Rick D. Russotto and Thomas P. Ackerman
• 1Department of Atmospheric Sciences, University of Washington, Seattle, WA, USA
• 2Joint Institute for the Study of the Atmosphere and Ocean, University of Washington, Seattle, WA, USA

Correspondence: Rick D. Russotto (russotto@uw.edu)

Abstract

The amount of solar constant reduction required to offset the global warming from an increase in atmospheric CO2 concentration is an interesting question with implications for assessing the feasibility of solar geoengineering scenarios and for improving our theoretical understanding of Earth's climate response to greenhouse gas and solar forcings. This study investigates this question by analyzing the results of 11 coupled atmosphere–ocean global climate models running experiment G1 of the Geoengineering Model Intercomparison Project, in which CO2 concentrations are abruptly quadrupled and the solar constant is simultaneously reduced by an amount tuned to maintain the top-of-atmosphere energy balance and pre-industrial global mean temperature. The required solar constant reduction in G1 is between 3.2 % and 5.0 %, depending on the model, and is uncorrelated with the models' equilibrium climate sensitivity, while a formula from the experiment specifications based on the models' effective CO2 forcing and planetary albedo is well correlated with but consistently underpredicts the required solar reduction. We propose an explanation for the required solar reduction based on CO2 instantaneous forcing and the sum of radiative adjustments to the combined CO2 and solar forcings. We quantify these radiative adjustments in G1 using established methods and explore changes in atmospheric temperature, humidity, and cloud fraction in order to understand the causes of these radiative adjustments.

The zonal mean temperature response in G1 exhibits cooling in the tropics and warming in high latitudes at the surface; greater cooling in the upper troposphere at all latitudes; and stratospheric cooling which is mainly due to the CO2 increase. Tropospheric specific humidity decreases due to the temperature decrease, while stratospheric humidity may increase or decrease depending on the model's temperature change in the tropical tropopause layer. Low cloud fraction decreases in all models in G1, an effect that is robust and widespread across ocean and vegetated land areas. We attribute this to a reduction in boundary layer inversion strength over the ocean, and a reduction in the release of water from plants due to the increased CO2. High cloud fraction increases in the global mean in most models. The low cloud fraction reduction and atmospheric temperature decrease have strong warming effects on the planet, due to reduced reflection of shortwave radiation and reduced emission of longwave radiation, respectively. About 50 % to 75 % of the temperature effect is caused by the stratospheric cooling, while the reduction in atmospheric humidity results in increased outgoing longwave radiation that roughly offsets the tropospheric temperature effect. The longwave (LW) effect of the cloud changes is small in the global mean, despite the increase in high cloud fraction. Taken together, the sum of the diagnosed radiative adjustments and the CO2 instantaneous forcing explains the required solar forcing in G1 to within about 6 %. The cloud fraction response to the G1 experiment raises interesting questions about cloud rapid adjustments and feedbacks under solar versus greenhouse forcings, which would be best explored in a model intercomparison framework with a solar-forcing-only experiment.

1 Introduction

In light of the warming of Earth in response to anthropogenic greenhouse gas emissions (IPCC2013), and continued lack of progress in curbing those emissions , some (e.g., Crutzen2006) have argued for serious consideration of solar geoengineering, or reflecting sunlight to artificially cool the Earth, as a means of reducing harms from climate change. The Geoengineering Model Intercomparison Project (GeoMIP; ) was created to study the climate impacts of solar geoengineering schemes. GeoMIP consists of a set of standardized experiments for global climate models (GCMs) that include both an increase in CO2 and some compensating effect, such as a reduction in the solar constant or an increase in stratospheric aerosol concentration. In experiment G1, the simplest of the GeoMIP experiments, the CO2 concentration is abruptly quadrupled relative to pre-industrial levels, as in the abrupt4xCO2 experiment from the Coupled Model Intercomparison Project, phase 5 (CMIP5; ), and at the same time the solar constant is abruptly reduced by an amount tuned to maintain top-of-atmosphere (TOA) energy balance and therefore keep the global mean temperature approximately at pre-industrial levels. Besides providing an important theoretical underpinning to the consideration of solar geoengineering scenarios, the G1 experiment is helpful for improving our fundamental understanding of how the climate responds differently to solar forcings, which operate in the shortwave (SW) part of the radiative spectrum versus greenhouse gas forcings, which operate in the longwave (LW), and how linear the response is to combinations of SW and LW forcings. This can help us understand paleoclimates in which the Sun was weaker (Feulner2012), attribution of climate change to anthropogenic as opposed to solar forcings , and the response of the climate to non-solar SW forcings such as aerosol forcings (Salzmann2016).

Table 1Models included in this study, with references, institutions, solar constant reduction in the G1 experiment (ΔS0), and global mean surface air temperature change in G1 – piControl (ΔT). All models have a full dynamical ocean coupled to the atmosphere.

For BNU-ESM, we are using a new realization, r3i1p1, that has a greater solar constant reduction and better compensates global mean temperature than the original. Two models that originally participated in G1, EC-Earth and HadCM3, are excluded from our analysis because many of the output fields necessary for this study were not available.

Figure 1Percent solar constant reduction for models running the G1 experiment versus (a) solar constant reduction predicted by Eq. (2), based on effective radiative forcing values from and pre-industrial planetary albedo values from , and (b) equilibrium climate sensitivity in the models, from . CESM-CAM5.1-FV and CSIRO-Mk3L-1-2 are excluded from this figure because these models were not included in .

An interesting question related to G1 is what amount of solar constant reduction $|\mathrm{\Delta }{S}_{\mathrm{0}}|$ is required to compensate for the CO2 increase. (For convenience, we hereafter drop the absolute value symbol and use ΔS0 to refer to the solar constant reduction, keeping in mind that the sign of the change is always negative in this context.) This quantity varies between about 3 % and 5 % depending on the model; the values for each model, which in every case achieved a global mean surface air temperature within 0.3 K of that in the CMIP5 pre-industrial control (piControl) experiment, are listed in Table 1. Because of its implications for the scale of the solar geoengineering intervention that would be required, it is important to understand what determines this quantity. We start our investigation of this question by plotting in Fig. 1a the required values of ΔS0 versus the values predicted by a simple formula based on matching the reduction in outgoing LW radiation (OLR) from the CO2 increase with a reduction in the absorbed SW radiation:

$\begin{array}{}\text{(1)}& \mathrm{\Delta }{S}_{\mathrm{0}}=\mathrm{4}×\frac{{F}_{\mathrm{4}\mathrm{xCO}\mathrm{2},\mathrm{eff}}}{\mathrm{1}-\mathit{\alpha }},\end{array}$

or, in percentage terms,

$\begin{array}{}\text{(2)}& \mathrm{\Delta }{S}_{\mathrm{0}}\left(\mathit{%}\right)=\left(\mathrm{4}×\frac{{F}_{\mathrm{4}\mathrm{xCO}\mathrm{2},\mathrm{eff}}}{\mathrm{1}-\mathit{\alpha }}\right)×\frac{\mathrm{100}\phantom{\rule{0.125em}{0ex}}\mathit{%}}{{S}_{\mathrm{0}}},\end{array}$

where S0 is the solar constant (about 1361 W m−2), α is the model's planetary albedo, and F4xCO2,eff is the effective radiative forcing from a CO2 quadrupling, calculated by regressing net TOA radiative flux against global mean temperature change in abrupt4xCO2 and taking the intercept . Figure 1a shows a strong correlation (correlation coefficient r=0.86) between the value of ΔS0 predicted by Eq. (2) and the value that actually achieved the experiment's objectives, indicating that CO2 forcing and planetary albedo determine ΔS0 to a first order (primarily forcing, since it varies much more between models than albedo does). However, for every model, the actual ΔS0 is greater than those predicted by this theory, as has been noted by for a subset of four models. This underprediction is relevant from a scenario modeling standpoint, since Eq. (1) was used by the modeling groups to create an initial guess for ΔS0 . Obtaining the correct value required running successive 10-year tuning runs of the GCMs, readjusting the solar reduction until a net TOA radiation imbalance of less than 0.1 W m−2 was achieved.

One factor not accounted for by the initial guess formula is climate feedbacks. We can get a sense for how feedbacks might affect the required ΔS0 by plotting it against equilibrium climate sensitivity (ECS), or the amount of global mean warming that occurs due to a doubling of CO2, the inter-model spread in which is primarily determined by feedbacks . Figure 1b shows that there is no correlation (correlation coefficient r=0.02) between these quantities. This makes sense because feedbacks are defined based on global mean temperature changes, which are zero by design (and close to zero in practice) in G1, and because the strengths of feedbacks are, at least to a first order, similar for different types of forcings . These results from GeoMIP corroborate those of , who found that the required geoengineering forcing is independent of climate sensitivity in experiments with an ocean GCM coupled to a single-layer atmosphere.

If neither radiative forcings nor feedbacks can fully explain the variation in the required ΔS0, then we must turn to radiative adjustments that do not depend on global mean temperature changes. The effective CO2 radiative forcing in Eq. (1) incorporates rapid adjustments of the atmosphere's temperature and humidity profiles, cloud properties, and surface albedo to the CO2 increase. However, such adjustments to the solar forcing are not accounted for. Effectively, Eq. (1) calculates the solar constant reduction that would balance the instantaneous CO2 increase if atmospheric properties were allowed to adjust to the CO2 increase but not to the solar constant reduction. The consistent underestimation of the required ΔS0 by Eq. (1) indicates that atmospheric and surface adjustments in response to the combined CO2 and solar instantaneous forcings have a greater net warming effect on the climate than such adjustments to the CO2 forcing alone, requiring a greater reduction in the solar constant to restore the global mean temperature to pre-industrial conditions.

While we cannot calculate rapid adjustments to the solar forcing alone without a set of model runs in which only the solar constant is changed, we can use the G1 output to calculate radiative adjustments to the combined CO2 and solar forcings, using existing analysis tools including the approximate partial radiation perturbation (APRP) method and radiative kernels . Assuming energy is conserved in the models and the analysis methods are reasonably accurate, it should be possible to use these calculated radiative adjustments to explain the required solar constant reduction in G1, as expressed in the following equation:

$\begin{array}{}\text{(3)}& \mathrm{\Delta }{S}_{\mathrm{0}}=\mathrm{4}×\frac{{F}_{\mathrm{4}\mathrm{xCO}\mathrm{2},\mathrm{inst}}+\sum \mathrm{\Delta }{R}_{X}}{\mathrm{1}-\mathit{\alpha }},\end{array}$

where F4xCO2,inst is the instantaneous radiative forcing from the CO2 quadrupling, which is the change in OLR from the CO2 increase when all atmospheric and surface properties are held constant , and ΔRX represents the global mean TOA radiative adjustments to the combined forcings associated with various physical properties X, following the notation of . Since there is no global mean temperature change in G1 by design (and approximately none in practice), we refer to the changes in TOA radiative balance resulting from changes in various physical properties of the atmosphere and surface as “adjustments” and not “feedbacks”. Note, however, that the changes in TOA radiation are in many ways dependent on local surface temperature changes, as discussed later.

This study examines changes in atmospheric temperature, specific humidity, cloud fraction, and surface albedo in G1, and quantifies the radiative effects of these changes in order to understand what determines the required ΔS0 and why it is greater than that predicted using effective CO2 forcing. We also explore the physical reasons for the changes in atmospheric properties, particularly cloud properties, which have been found to strongly affect meridional energy transport changes in G1, with implications for regional temperature and precipitation responses . The changes in atmospheric properties, including clouds, are plotted and discussed in Sect. 2. Section 3 quantifies the radiative effects of these surface and atmospheric adjustments to the G1 forcing. Section 4 examines the global means of these adjustments to see which are most important in determining the required ΔS0 according to Eq. (3). In Sect. 5, we summarize our results and discuss implications for future research on geoengineering and solar climate forcings.

Figure 2Zonal mean temperature change for G1 – piControl in each model as a function of pressure.

2 Changes in the physical state of the atmosphere

To understand the physical basis for the radiative adjustments calculated in later sections, in this section, we show changes in atmospheric temperature, specific humidity, and cloud fraction that occur in the G1 experiment relative to pre-industrial conditions. Throughout the paper, we show averages over 40-year time periods: years 11–50 of the G1 simulation, to avoid incorporating transient effects that occur in the first 10 years into averages, and years 1–40 of the piControl simulation, except where otherwise noted. Averaging over years 11–50 is standard procedure for analysis of the GeoMIP experiments (e.g., Kravitz et al.2013a); a longer averaging period would not be possible since most models stopped the experiment after 50 years. We treat years 11–50 mean as equilibrium response, which seems appropriate since all components of the surface energy budget show little to no drift after the first 10 years . We also plotted time series of the SW radiative adjustments calculated in Sect. 3 (Fig. S13 in the Supplement) and found no appreciable drift that would have extended beyond 50 years in any of the models.

Figure 2 shows the zonal mean temperature change for G1 – piControl in each of the 11 models listed in Table 1. Several features common to all models are apparent. First, while the global mean surface air temperatures are all within 0.3 K of pre-industrial levels (Table 1), all of the models exhibit surface cooling in the tropics and warming in the polar regions. This phenomenon has long been noted as a feature of climate model experiments with the G1 setup and is due to the imposition of a net negative forcing in the tropics and a net positive forcing at the poles . However, cooling dominates when considering the atmosphere as a whole. The tropical mid- to upper troposphere cools more than the surface does, because the tropical temperature profile tends to follow a moist adiabat (e.g., Wetherald and Manabe1975), so that slight cooling at the surface leads to greater cooling aloft. The cooling of the tropical upper troposphere mirrors the effect that happens in global warming, where the upper troposphere warms more than the surface and emits more LW radiation, leading to a negative climate feedback known as the lapse rate feedback. In the case of G1, reduced LW emission from the atmospheric cooling has a warming effect on the planet; we quantify this effect using radiative kernels in Sect. 3.2.

Figure 3Zonal mean change in the natural log of specific humidity for G1 – piControl in each model as a function of pressure.

Most models have an area of reduced cooling or even warming in the tropics near 100 hPa. This corresponds to the location of the tropical tropopause layer (TTL), an area in the tropics between about 70 and 150 hPa with properties of both the troposphere and stratosphere . The detailed vertical structure of temperature changes here may have to do with complex interactions between local temperature, humidity, and cloud properties. Another notable feature of the temperature change is the cooling of the stratosphere. An increase in carbon dioxide concentration cools the stratosphere, due to increased emission of LW radiation to space , and a decrease in the solar constant also cools the stratosphere because it reduces the amount of ultraviolet radiation absorbed by ozone. The stratospheric cooling effect from the solar constant reduction is about an order of magnitude smaller than that from the CO2 quadrupling .

Figure 4Zonal mean change in cloud fraction for G1 – piControl in each model as a function of pressure or height for HadGEM2-ES. To help comparisons with other models, the vertical axis for HadGEM2-ES is scaled according to ${e}^{-z/\mathrm{8000}\phantom{\rule{0.125em}{0ex}}\mathrm{m}}$ (where z is height), which is approximately proportional to pressure.

Figure 3 shows the change in the natural log of specific humidity between G1 and piControl in each model. We use a log scale because it makes it easier to visualize changes in specific humidity that occur over multiple orders of magnitude, and because log humidity changes are used in the water vapor radiative kernel calculations described in Sect. 3.2. Most of the troposphere becomes drier in G1 in all models, consistent with the large-scale cooling given similar relative humidity. Since water vapor is a strong greenhouse gas, this drying has a cooling effect on the planet, which we quantify in Sect. 3.2. Most models show moistening in the polar regions at low altitudes, consistent with the warming there, although the moistening is typically confined to smaller areas than the warming, indicative of a slight decrease in relative humidity at the poles (see Fig. 5 of ). Interestingly, stratospheric water vapor decreases in most models, but it increases in the three models (BNU-ESM, CSIRO-Mk3L-1-2, and IPSL-CM5A-LR) that have warming in the TTL (albeit this moistening is mostly confined to the Northern Hemisphere in the IPSL model). This is consistent with stratospheric humidity being set by temperatures in the TTL, through which air travels to reach the stratosphere as part of the Brewer–Dobson circulation (e.g., Brewer1949; Newell and Gould-Stewart1981).

Figure 4 shows the zonal mean changes in cloud fraction in each of the models for G1 – piControl. Unlike atmospheric temperature and humidity, cloud fraction model output in CMIP5 and GeoMIP was archived on the native model vertical grid instead of a set of standardized pressure levels. Most of the GeoMIP models use hybrid sigma pressure coordinates, with the exceptions of GISS-E2-R, which uses pressure coordinates, and HadGEM2-ES, which uses hybrid sigma height coordinates. To enable direct comparisons with the temperature and humidity changes and radiative kernel calculations, we have regridded the cloud fraction output to the standard CMIP5 pressure levels or to a fixed height grid for HadGEM2-ES. Conversion from hybrid sigma to pressure or height coordinates was done using a Python function (see “Code and data availability” below) based on the algorithm used in the “convert_sigma_to_pres” Matlab function by , available at http://www.aos.wisc.edu/~dvimont/matlab/. Since surface pressure output (required for the hybrid sigma pressure regridding) was only available for the last 50 years of the piControl simulation for CSIRO-Mk3L-1-2, we have used the last 40 years of this simulation as the control case for cloud fraction for this model, instead of the first 40 years.

In their study of four models running G1, noted that all four had a reduction in low cloud fraction, while high clouds had an inconsistent change. Figure 4 shows that an overall reduction of low cloud fraction occurs in all 11 models included in this study. For high clouds, we also find an inconsistent response, but overall high cloud fraction increases in most models. Some models, especially those in which the TTL warms (Fig. 2), have a decrease in high cloud fraction in the TTL, and two of them, CSIRO-Mk3L-1-2 and IPSL-CM5A-LR, have an overall decrease in high cloud fraction. Since low clouds primarily have a cooling effect on the climate due to their strong SW reflection, a reduction in low clouds would result in a warming effect that would partially offset the cooling from solar geoengineering. An increase in high cloud fraction would also be expected to have a warming effect on the planet by reducing LW emission to space, although other variables, such as cloud height, are more important to the LW effect of cloud changes in global warming simulations . We quantify the TOA SW and LW effects of the changes in cloud properties in Sect. 3.1 and 3.2, respectively. In many models, there is an increase in clouds in the stratosphere over Antarctica, likely due to the stratospheric cooling. Two models, HadGEM2-ES and MIROC-ESM, have a dipole in cloud fraction changes in the upper troposphere, corresponding to northward and southward shifts, respectively, of the intertropical convergence zone (ITCZ) in these models .

To get a sense of the zonally asymmetric spatial patterns of cloud fraction changes and to better understand areas of inter-model consensus and disagreement, we plot in Fig. 5 maps of the multi-model mean changes in low, middle, and high cloud fraction for G1 – piControl. Within the ranges for low, middle, and high clouds, we assume random overlap between adjacent layers of the common pressure grid. We use 680 hPa as the boundary between low and middle clouds and 440 hPa as the boundary between middle and high clouds, following the standards for the International Satellite Cloud Climatology Project (ISCCP; see Fig. 2 of ), or 3250 and 6500 m in the case of HadGEM2-ES, which roughly correspond to these pressure levels in the 1976 Standard Atmosphere (NOAA1976). These plots, and all subsequent multi-model mean maps, show stippling where fewer than all but two of the included models agree on the sign of the change, so that unstippled areas indicate robust changes. Since this agreement could happen by chance in isolated areas, we focus on areas with apparent spatial structure or a physical reason why we might expect a change. For all multi-model mean maps, corresponding maps for each of the individual models are available in the Supplement. Global mean cloud fraction changes for the individual models are shown in Table 2.

Figure 5Multi-model mean changes in low (a), middle (b), and high (c) cloud fraction for G1 – piControl. Hatching indicates areas where fewer than 9 of the 11 models agree on the sign of the change.

Table 2Global mean changes in low, middle, and high cloud fraction in G1 – piControl.

The reduction in low cloud fraction (Fig. 5a) is widespread, occurring over most ocean areas, except for regions close to the Equator and poles, and over most non-desert land areas. Middle clouds (Fig. 5b) have fewer areas with robust changes, but there is a reduction in the cloud fraction on either side of the Equator over the Atlantic and Pacific and over the equatorial Indian Ocean. This may be related to a narrowing of the annual mean tropical precipitation maximum (see Fig. 5 of Tilmes et al.2013), which may be due in part to a reduction in the seasonal migration of the ITCZ . For high clouds (Fig. 5c), there are few areas with robust changes, but there is a notable increase in high clouds over the Equator, in some subtropical regions (around 30 N and S), and over the poles, particularly Antarctica. Figure 4 shows that the high cloud increases over the poles are mostly in the stratosphere.

Without additional experiments varying potential drivers of cloud changes, it is difficult to prove definitively the causes for the changes in cloud fraction. However, it is possible to gain some insight into the reasons for changes in low cloud fraction over the ocean by plotting several variables that are correlated with low cloud fraction in observations. These include lower-tropospheric stability (LTS), defined as the difference in potential temperature between 700 hPa and the surface , and estimated inversion strength (EIS), a metric of the temperature inversion at the top of the marine boundary layer. EIS is defined as (Wood and Bretherton2006, Eq. 4)

$\begin{array}{}\text{(4)}& \mathrm{EIS}=\mathrm{LTS}-{\mathrm{\Gamma }}_{\mathrm{m}}^{\mathrm{850}}\left({z}_{\mathrm{700}}-\mathrm{LCL}\right),\end{array}$

where ${\mathrm{\Gamma }}_{\mathrm{m}}^{\mathrm{850}}$ is the moist adiabatic lapse rate at 850 hPa, z700 is the height of the 700 hPa surface, and LCL is the lifting condensation level.

Figure 6 shows the changes in EIS (Fig. 6a) and LTS (Fig. 6b) for G1 – piControl. Both of these quantities generally decrease across most of the ocean, except for some regions centered near 15 N and S. The reduction in EIS is generally smaller than the reduction in LTS (due to the correction for the moist adiabatic temperature profile) but is still widespread. A reduction of the strength of the inversion at the top of the boundary layer would be expected to reduce low cloud fraction by encouraging mixing of dry air into the boundary layer, so the reduction in EIS over the ocean is a likely explanation for the reduction in low cloud fraction there. Stability metrics are included in low cloud fraction schemes in many models, and those that use the scheme, such as CCSM4 and NorESM1-M, have an explicit dependence of low cloud fraction on stability. However, the robustness of the reduction in low cloud fraction in G1 indicates that it is not the result of the idiosyncrasies of any one cloud fraction scheme.

Figure 6Multi-model mean changes in EIS (a) and LTS (b) for G1 – piControl. Hatching indicates areas where fewer than seven of nine models agree on the sign of the change. CSIRO-Mk3L-1-2 and MPI-ESM-LR models are excluded from this plot because near-surface specific humidity output, which is required to calculate EIS, was not available.

Besides changes in stability metrics, other factors that have been suggested as explaining changes in marine stratocumulus cloud fraction under global warming conditions in large-eddy simulation models include reduced LW radiative cooling from cloud tops due to increased CO2 and H2O concentrations, decreased subsidence above the boundary layer, and increased sea surface temperatures . analyzed changes in marine stratiform cloud fraction in CMIP3 and CMIP5 global warming experiments, and found a reduced low cloud fraction in most models, which they attributed to an increase in sea surface temperature (SST). While EIS increased in the global warming experiments, which would promote increased cloud fraction, this was not enough to compensate for the SST increase. In G1, SST changes little (and in fact decreases slightly in the tropics and subtropics; Hong et al.2017, Fig. 1), leaving EIS to dominate changes in low cloud fraction over the ocean.

It does not appear that cloud top radiation or subsidence could be responsible for the widespread low cloud reduction for the following reasons. The mechanism of reduced LW radiative cooling from cloud tops would be much weaker for G1 than for global warming if at all present because, while CO2 concentrations have increased, water vapor concentrations have decreased; also, the reduction in insolation further reduces the net radiative cooling rate via its direct SW effect. We have not tried to quantify how these fluxes have changed in G1 since LW radiative fluxes at the top of the boundary layer were not included in the GeoMIP model output archive. We might expect that subsidence would change due to the effects of the combined CO2 and solar forcings on the atmospheric radiative cooling profile. However, meridional stream function anomaly plots for G1 – piControl show that while some areas have anomalous subsidence, others have anomalous rising motion, and these regions are not consistent between models or with the regions of low cloud fraction decrease. Large-eddy simulation experiments involving a CO2 increase and insolation reduction could help better understand what role, if any, these processes play in the changes in low cloud fraction in the G1 scenario, as well as the role of any changes in boundary layer or free troposphere relative humidity not associated with any of the processes discussed here.

attribute the increase in EIS in global warming experiments to greater surface warming over the continents and the tropical western Pacific warm pool relative to the rest of the ocean; the warmed air is then advected over the tops of the marine stratocumulus fields. However, a reverse version of this mechanism does not seem to be at work in G1 because cooling is more robust over the ocean than over land (Kravitz et al.2013a, Fig. 2). It is also important to keep in mind that there are different metrics of stability that are useful for different parts of the atmosphere and for different types of clouds. argued that any cloud cover changes in G1 would be due in part to increases in atmospheric stability, but in our study it appears to be a decrease in stability that is most relevant to the low cloud reduction. Another metric of stability, the rate of increase of equivalent potential temperature θe with height, does in fact increase in G1 relative to piControl, as shown in Fig. 8 of . So, even as the atmosphere has gotten less stable in G1 with respect to boundary layer turbulence, it has gotten more stable with respect to deep convection, at least to the extent to which $\partial {\mathit{\theta }}_{\mathrm{e}}/\partial z$ is a predictor of changes in deep convection, as assumed by . To better understand the reasons for the changes in clouds, it would be useful to further investigate the effects of CO2 and solar forcings on potential and equivalent potential temperature profiles.

Over land, existing research suggests that the reduction in low cloud fraction in G1 is a result of the physiological responses of plants to increased CO2, as represented in the models' dynamic vegetation schemes. ran GCM simulations in which the CO2 concentrations experienced by plants were doubled while the radiative fluxes were held constant, and found that low cloud fraction decreased in many vegetated land areas (see their Fig. 1, central panel). The low cloud fraction decrease in the Cao et al. study is strongest in South America, eastern North America, southeast Asia, southeast Africa, and western Europe, which are the same areas of reduced low cloud cover in G1. The mechanism is that, when CO2 concentrations are higher, plants' stomata do not need to open as much to take in the same amount of CO2, leading to less transpiration of water from the plants . This causes a reduction in near-surface relative humidity over land, seen in both Cao et al. (2010, Fig. 2) and G1 (Smyth et al.2017, Fig. 5), which reduces the cloud fraction. In addition to plant physiology, it is possible that some of the reduction in relative humidity and cloud fraction over land in G1 is due to a reduction in evaporation directly caused by the reduction in surface SW radiation. The balance between these two quantities explains the reduction in global mean precipitation in G1 , since precipitation must balance evaporation, suggesting that a similar mechanism may affect cloud fraction. Over the ocean, however, near-surface relative humidity increases in G1 in most areas, despite the reduction in evaporation , implying that evaporation changes are not the reason for the low cloud changes there.

Table 3Global mean radiative adjustments in G1 – piControl, and excess and total solar forcing in G1, in W m−2. Positive values indicate a warming effect (increase in absorbed SW radiation or decrease in OLR), except for solar forcing where positive values represent a cooling. SW adjustments correspond to multi-model means plotted in Fig. 7. LW adjustments correspond to multi-model means plotted in Figs. 8 and 9, with the sign flipped for Fig. 8. “Sum” is the sum of all the SW and LW adjustments. Fexcess is calculated using Eq. (6) and represents the actual instantaneous solar forcing (Fsolar) in G1 minus that which would match the CO2 effective or instantaneous forcing. Fsolar represents the total instantaneous solar forcing calculated from theory (Eq. 8) or actually used in G1 (Eq. 9).

To calculate the SW radiative effects of changes in clouds and other atmospheric and surface properties, we use the APRP method introduced by , which is based on a single-layer radiative transfer model of the atmosphere that can be expressed analytically and requires as inputs only the monthly mean surface and TOA radiative fluxes and total column cloud fraction outputs from the GCMs. APRP shows the radiative effects of physical changes in clouds, accounting for cloud masking effects, in which the differences between clear-sky and all-sky fluxes change in response to forcing without changes in the clouds themselves. The calculations shown here have previously been used as inputs to energy balance model simulations to understand the effects of changes in clouds and surface albedo on atmospheric energy transport in G1 .

Figure 7 shows the multi-model mean change in net downward SW radiative flux at the TOA due to changes in clouds (Fig. 7a), non-cloud atmospheric scattering and absorption (Fig. 7b), and surface albedo (Fig. 7c), calculated using APRP. Global mean radiative adjustments for the individual models in the SW and LW are shown in Table 3, which will be referred to in the discussion of the required solar forcing in G1 in Sect. 4. Clouds generally have a robust and widespread warming effect in the SW, in locations that closely correspond to the areas of reduced low cloud fraction shown in Fig. 5a. The non-cloud atmosphere effects are very weak by comparison in the multi-model mean, but there are several models with appreciable positive values for this adjustment. Maps of this adjustment for the individual models (Fig. S7) show that for HadGEM2-ES, it appears to be related to a reduction in atmospheric dust, since most of the warming effect occurs over and downwind of deserts; in IPSL-CM5A-LR, the effect is relatively spatially uniform but slightly stronger in higher latitudes. For surface albedo, there are warming effects in high latitudes from decreases in sea ice and snow cover associated with the residual polar warming in G1. There are also some warming effects in lower latitudes near desert regions, such as in the Sahel region; this may have to do with vegetation effects. There are several small regions, such as Tibet, with increases in surface albedo, presumably due to increased snow cover as a result of surface cooling there (see Fig. 2 of ). Surface albedo effects are strong in some locations, such as the Sea of Okhotsk, but the relatively small area over which surface albedo changes can occur limits their importance in the global mean.

Figure 7Multi-model mean change in net downward SW radiation at the TOA in G1 – piControl due to changes in cloud properties (a), non-cloud atmospheric absorption and scattering (b), and surface albedo (c), calculated using APRP method . Hatching indicates areas where fewer than seven of nine models agree on the sign of the change. CSIRO-Mk3L-1-2 and GISS-E2-R models are excluded because not all fields necessary for APRP were correctly archived.

The technique of radiative kernels was developed to quantify LW radiative adjustments and feedbacks using standard monthly mean climate model output. These kernels consist of matrices of the partial derivatives of OLR with respect to changes in surface temperature, atmospheric temperature, specific humidity, and greenhouse gas concentration as a function of latitude, longitude, month, and (where applicable) pressure, calculated using offline calculations with a particular GCM's radiative transfer code. Radiative kernels have been developed based on a variety of GCMs, including GFDL AM2 , CAM3 , MPI-ESM-LR , and CESM-CAM5 .

We have applied the radiative kernels to the G1 ensemble. The choice of model used to generate the kernels has been shown to have little effect on the results . After regridding the kernels to the latitude and longitude grid of each GCM, we multiplied them by the changes in temperature and the log of specific humidity, normalized by the standard anomaly used to compute the kernels (1 K for the surface and atmospheric temperature kernels, and the change in log specific humidity associated with a 1 K warming at constant relative humidity for the water vapor kernel), in order to compute the change in OLR associated with the changes in each of these quantities for G1 – piControl. We summed the OLR changes from each vertical level in order to get overall radiative adjustments from column temperature and water vapor changes, and we used the annual mean of the monthly results for our analysis.

Figure 8 shows multi-model mean changes in OLR for G1 – piControl calculated from the atmospheric temperature (Fig. 8a), surface temperature (Fig. 8b), and water vapor (Fig. 8c) kernels. Global means for the individual models are shown in Table 3. For the atmospheric temperature kernel, there is a strong decrease in OLR that is widespread across the globe and robust across models. This is associated with the cooling of the atmosphere (see Fig. 2) and reduced longwave emission. The reduction in OLR is stronger in the tropics than in the polar regions and is due to some combination of upper tropospheric and stratospheric cooling. We discuss the contribution of the stratospheric component in the next section. Surface temperature changes have little effect on the TOA LW radiation balance, but there is a reduction in OLR in the tropics and subtropics and an increase in the polar regions that is consistent across models, due to the patterns of tropical cooling and polar warming at the surface. The OLR change from the surface temperature kernel is much smaller than that for atmospheric temperature because the atmosphere is not very transparent to LW radiation in most wavelengths, and because temperature changes are smaller at the surface than in the upper troposphere and stratosphere. Changes in water vapor concentration cause a robust increase in OLR that partially offsets the decrease in OLR from the atmospheric temperature kernel. The water vapor concentration decreases in the upper troposphere (Fig. 3), which increases LW emission to space by lowering the effective altitude of emission.

Figure 8Multi-model mean change in OLR in G1 – piControl due to changes in atmospheric temperature (a), surface temperature (b), and specific humidity (c), calculated using radiative kernels . Hatching indicates areas where fewer than 9 of 11 models agree on the sign of the change.

In addition to the quantities plotted in Fig. 8, radiative kernels can also be used to calculate the effect of changes in cloud properties on OLR. This is often measured according to the change in the cloud radiative effect (CRE), which is the difference in OLR in clear-sky minus all-sky averages. However, changes in the cloud radiative effect may include cloud masking effects. We can correct the change in LW CRE for the effects of existing clouds on clear-sky fluxes using the difference in flux changes calculated according to clear-sky and all-sky kernels, following :

$\begin{array}{ll}& \mathrm{\Delta }{\mathrm{LWCRE}}_{\mathrm{adjusted}}={\mathrm{LWCRE}}_{\mathrm{G}\mathrm{1}}-{\mathrm{LWCRE}}_{\mathrm{piControl}}\\ & \phantom{\rule{1em}{0ex}}+\left(\mathrm{\Delta }{\mathrm{OLR}}_{k,T}-\mathrm{\Delta }{\mathrm{OLR}}_{k,T,\mathrm{clear}}+\mathrm{\Delta }{\mathrm{OLR}}_{k,{T}_{\mathrm{s}}}\right\\ & \phantom{\rule{1em}{0ex}}-\mathrm{\Delta }{\mathrm{OLR}}_{k,{T}_{\mathrm{s}},\mathrm{clear}}+\mathrm{\Delta }{\mathrm{OLR}}_{k,q}-\mathrm{\Delta }{\mathrm{OLR}}_{k,q,\mathrm{clear}}\\ \text{(5)}& & \phantom{\rule{1em}{0ex}}+\mathrm{\Delta }{\mathrm{OLR}}_{k,{\mathrm{CO}}_{\mathrm{2}}}-\mathrm{\Delta }{\mathrm{OLR}}_{k,{\mathrm{CO}}_{\mathrm{2}},\mathrm{clear}}),\end{array}$

where, in the subscripts, k denotes a change in OLR calculated using a kernel, clear denotes quantities calculated using the clear-sky instead of all-sky kernels, T is atmospheric temperature, Ts is surface temperature, and q is specific humidity. Since the CO2 forcing kernels were for a doubling of CO2, we doubled these kernels to obtain the radiative flux changes for a CO2 quadrupling.

Figure 9 shows the multi-model mean change in LW CRE calculated using Eq. (5). There is a modest cooling effect in the global, multi-model mean (see also Table 3), but there are some places where there is a robust warming effect. The strongest warming effects occur near the eastern equatorial oceans, where the increase in high cloud fraction is greatest, while the strongest cooling effects occur in two belts in the eastern Pacific, which are associated with robust decreases in low and middle cloud fraction (see Fig. 5). There are also widespread cooling effects over the midlatitude oceans, where low cloud fraction decreases. Generally, an increase in high cloud fraction would be expected to result in a warming effect, because high clouds are much cooler than the surface and are more effective at trapping LW radiation. However, in the case of G1, it appears that the LW effect of the decrease in low cloud fraction compensates for this, despite the cloud temperature being closer to the surface temperature, because the low cloud reduction occurs over a wide area. The spatial correspondence of areas of strong cooling effects in Fig. 9 to areas of strong low cloud fraction decrease in Fig. 5a supports this view. Besides cloud fraction, LW radiation is also sensitive to changes in cloud height and cloud optical depth . It may be that the global mean increase in high cloud fraction that occurs in most models has a limited effect on OLR because the new clouds being formed are optically thin; we would especially expect this in the case of polar stratospheric clouds. The radiative effects of changes in cloud optical thickness are difficult to assess from the GeoMIP output currently available. These effects have been quantified in global warming simulations using cloud radiative kernels , but the use of these requires cloud fraction statistics binned by optical depth and cloud top height produced by the ISCCP satellite simulator that is part of the Cloud Feedback Model Intercomparison Project (CFMIP; Bony et al.2011) Observation Simulator Package . The simulator must be run inline with each GCM or else requires instantaneous cloud fraction output (rather than monthly means) in order to be run retrospectively. The necessary outputs for cloud radiative kernels were saved in CFMIP but not in GeoMIP. It would be useful to follow the CFMIP protocols in future GeoMIP experiments in order to allow further quantitative analysis of the changes in clouds that occur under combined SW and LW forcings.

Figure 9Multi-model mean change in LW cloud radiative effect in G1 – piControl, corrected for cloud masking of LW air temperature, surface temperature, and water vapor adjustments and CO2 forcing. Positive values indicate a decrease in OLR, i.e., a warming effect. Hatching indicates areas where fewer than 9 of 11 models agree on the sign of the change.

4 Connections between radiative effects and required solar reduction

Having quantified the radiative effects of changes in the physical properties of the atmosphere and surface in G1, we now revisit the question of the amount of solar constant reduction required to offset the quadrupling of CO2. The solar constant reduction predicted based on effective CO2 radiative forcing (Eq. 1) systematically underestimated the actual reduction required (Fig. 1b). In this section, we attempt to account for this discrepancy by comparing the amount of extra solar forcing needed with the global means of the radiative adjustments calculated in Sect. 3. This comparison is shown in Fig. 10 for the eight models for which effective radiative forcing values from were available and all of the radiative adjustments could be calculated. The excess required solar reduction, Fexcess, shown in black, is calculated according to

$\begin{array}{ll}{F}_{\mathrm{excess}}=& \phantom{\rule{0.125em}{0ex}}\left(\mathrm{\Delta }{S}_{\mathrm{0}}\left(\mathit{%}{\right)}_{\mathrm{actual}}-\mathrm{\Delta }{S}_{\mathrm{0}}\left(\mathit{%}{\right)}_{\mathrm{predicted}}\right)\\ \text{(6)}& & ×\frac{\mathrm{1361}\phantom{\rule{0.125em}{0ex}}\mathrm{W}\phantom{\rule{0.125em}{0ex}}{\mathrm{m}}^{-\mathrm{2}}}{\mathrm{100}\phantom{\rule{0.125em}{0ex}}\mathit{%}}×\frac{\mathrm{1}-\mathit{\alpha }}{\mathrm{4}},\end{array}$

where ΔS0(%)actual is listed in Table 1 and ΔS0(%)predicted is calculated using Eq. (2). In terms of radiative forcing, Fexcess is the difference between the actual solar forcing required in G1 and the effective forcing from the CO2 quadrupling.

The relative sizes of the bars in Fig. 10 are fairly similar across models. The strongest warming effect is generally from the LW atmospheric temperature adjustment, followed by the SW cloud adjustment. The only consistent cooling effect comes from the LW water vapor adjustment. Surface albedo effects are generally small, as is the SW clear-sky adjustment, with the exceptions discussed in Sect. 3.1. The LW surface temperature adjustment is practically negligible in all models, while the LW cloud adjustment is also small but has an inter-model range of about 1 W m−2. The model with the greatest cooling effect from the LW cloud adjustment, IPSL-CM5A-LR, is the model with the greatest global mean decrease in high cloud fraction, whereas most other models have an increase in high cloud fraction (Table 2).

Figure 11As in Fig. 10 but with excess solar forcing calculated using instantaneous instead of effective CO2 radiative forcing. The navy blue bar indicates the reduction in OLR due to stratospheric temperature adjustment from CO2 quadrupling given by , to illustrate the portion of the atmospheric temperature adjustment to G1 attributable to stratospheric cooling.

To account for this, we plot in Fig. 11 the same quantities as in Fig. 10 but where the black bars are calculated using instantaneous rather than effective CO2 forcing for the predicted solar constant reduction (i.e., using F4xCO2,inst rather than F4xCO2,eff in Eq. 2 and then substituting into Eq. 6). Expressed mathematically, the comparison done in Fig. 11 is

$\begin{array}{ll}& \left(\left(\mathrm{\Delta }{S}_{\mathrm{0}}\left(\mathit{%}{\right)}_{\mathrm{actual}}\right)×\frac{\mathrm{1361}\phantom{\rule{0.125em}{0ex}}\mathrm{W}\phantom{\rule{0.125em}{0ex}}{\mathrm{m}}^{-\mathrm{2}}}{\mathrm{100}\phantom{\rule{0.125em}{0ex}}\mathit{%}}-\mathrm{4}×\frac{{F}_{\mathrm{4}\mathrm{xCO}\mathrm{2},\mathrm{inst}}}{\mathrm{1}-\mathit{\alpha }}\right)\\ \text{(7)}& & \phantom{\rule{1em}{0ex}}×\frac{\mathrm{1}-\mathit{\alpha }}{\mathrm{4}}\phantom{\rule{0.25em}{0ex}}\stackrel{?}{=}\phantom{\rule{0.25em}{0ex}}\sum \mathrm{\Delta }{R}_{X}.\end{array}$

The black bars in Fig. 11 show the left-hand side of the Eq. (7), while the gray bars show the right-hand side. If the two bars are the same size, that means that the actual solar constant reduction matches that from Eq. (3).

Instantaneous forcing, unlike effective forcing, cannot be calculated from monthly mean model output through a simple linear regression of TOA flux changes against surface temperature; instead it requires running each GCM's radiative transfer code offline with standard and quadrupled CO2 concentrations. For this reason, estimates of instantaneous CO2 forcing are available for fewer models than for effective forcing. We used the “double call” instantaneous forcing estimates from the CMIP5 archive shown in for the CanESM-2 and IPSL-CM5A-LR models. For three other models (CCSM4, HadGEM2-ES, and NorESM1-M), we use estimates of instantaneous CO2 forcing given by based on residuals between total TOA flux changes and radiative responses calculated with radiative kernels.

In Fig. 11, the black and gray bars match to within about 10 %, indicating that the theory expressed in Eq. (3) works well for explaining the amount of solar constant reduction required to balance a CO2 increase. Since the equation must be true given energy conservation, this agreement demonstrates that the approximate methods used to calculate the radiative adjustments work well in the context of G1. In evaluating this agreement, it is useful to express Eq. (3) in terms of total instantaneous solar forcing rather than solar constant reduction:

$\begin{array}{}\text{(8)}& {F}_{\mathrm{solar},\mathrm{theory}}={F}_{\mathrm{4}\mathrm{xCO}\mathrm{2},\mathrm{inst}}+\sum \mathrm{\Delta }{R}_{X},\end{array}$

and compare it to the actual solar forcing in G1:

$\begin{array}{}\text{(9)}& {F}_{\mathrm{solar},\mathrm{actual}}=\mathrm{\Delta }{S}_{\mathrm{0},\mathrm{actual}}\left(\mathit{%}\right)×\frac{\mathrm{1361}\phantom{\rule{0.125em}{0ex}}\mathrm{W}\phantom{\rule{0.125em}{0ex}}{\mathrm{m}}^{-\mathrm{2}}}{\mathrm{100}\phantom{\rule{0.125em}{0ex}}\mathit{%}}×\frac{\mathrm{1}-\mathit{\alpha }}{\mathrm{4}}.\end{array}$

These values are listed in the last two columns of Table 3. The errors in the total solar forcing in G1 obtained from Eq. (8) are all within 0.5 W m−2 or within about 6 % of the total, indicating that the instantaneous solar forcing required to balance an abrupt CO2 increase is well explained by the sum of the instantaneous CO2 forcing and the radiative adjustments to the combined forcings.

5 Conclusions

This paper characterizes the physical responses of the atmosphere and surface to the GeoMIP G1 scenario and quantifies their radiative effects, with the goal of explaining what determines the solar constant reduction required to balance the CO2 increase. At the surface, the tropics cool and the poles warm while global mean temperature remains at pre-industrial conditions. The upper troposphere experiences cooling at all latitudes, with the tropical upper troposphere cooling more than the surface. The stratosphere cools more than anywhere else in the atmosphere, due primarily to the CO2 increase . The tropospheric temperature effect is a reversal of the negative lapse rate feedback that happens in global warming simulations, in which the tropical upper troposphere warms more than the surface; in G1, because the tropics cool and the tropical temperature profile tends to follow a moist adiabat, the upper troposphere also cools, which has a warming effect on the climate by reducing OLR. Atmospheric specific humidity is reduced in the upper troposphere, which makes the atmosphere less opaque to LW radiation and largely offsets the radiative effect of the tropospheric cooling. Low cloud fraction exhibits a widespread decrease over the ocean and vegetated land areas in all models, which we attribute to decreases in boundary layer inversion strength over the ocean and reduced evaporation from plants due to the physiological response to increased CO2 over land. The low cloud fraction reduction has a strong surface warming effect due to reduced reflection of sunlight by the clouds. High cloud fraction increases in the global mean in most models, but the LW radiative effect of cloud changes in G1 is slightly negative in the global, multi-model mean. When all the global mean radiative adjustments in G1 are added together, the results account, to within 10 %, for the difference between the solar constant reduction that would match the instantaneous CO2 forcing and the tuned solar constant reduction that met the TOA energy balance threshold required by the G1 experiment protocol.

For future model runs of the G1 experiment, such as those being prepared for the next phase of GeoMIP corresponding to CMIP6 , it would be useful to have a better initial guess for the solar constant reduction in order to reduce the necessary amount of tuning. Using Eq. (3) for this purpose would be tricky because the radiative responses to the combined CO2 and solar forcings would be unknown before actually running the model. However, one could simply substitute an empirical value of about 4 W m−2, a typical value for the sum of the radiative adjustments in G1 (Fig. 10), for ∑ΔRX in Eq. (3). Then, tuning would only need to account for model-specific deviations from this number. If instantaneous CO2 forcing was not available for a particular model, the modelers could add a correction of about 2.5 to 3 W m−2, a typical value for the black bars in Fig. 10, to the effective CO2 forcing in Eq. (1).

It would be very interesting to study how cloud rapid adjustments and feedbacks differ under solar versus CO2 forcing in a model intercomparison framework. The cloud fraction changes in G1 imply that rapid cloud responses to CO2 and solar forcings are different, but this requires further study with GCM runs that perturb only the solar constant and not CO2. Since the global mean temperature does not change, the G1 experiment tells us very little about cloud feedbacks, which are temperature dependent. An attempt was made to study cloud rapid adjustments and feedbacks under solar forcings by subtracting the G1 experiment from the abrupt4xCO2 experiment, but this approach is bound to produce similar feedback parameters for this “solar” forcing versus the abrupt4xCO2 – piControl CO2 forcing because, while there are two different baselines, there is only one perturbation run, abrupt4xCO2, that has a global mean temperature change onto which radiative flux changes can be regressed. Some studies have included solar-only GCM runs , but these have included only one or two models, and while some, such as , have looked at cloud radiative effects and cloud fraction, none have used methods that account for cloud masking to isolate the radiative effects of physical cloud changes. There is no solar equivalent of abrupt4xCO2 in CMIP5 or any of its associated projects; the closest analogue is probably the aerosol-forcing-only historical runs from the CMIP5 “historicalMisc” collection, analyzed, e.g., by . The Precipitation Driver and Response Model Intercomparison Project includes a solar constant increase experiment, and the CFMIP component of CMIP6 will include abrupt solar constant increase and decrease runs . These ensembles will provide good opportunities to further explore cloud and other changes under solar forcings.

Besides their effects on the required solar forcing, the changes in atmospheric physical properties that occur in G1 are interesting in their own right and may have policy implications if they translated to a real geoengineering deployment. If low cloud fraction were actually reduced by solar geoengineering, it could result in increased solar energy production, and could enhance vegetation growth in sunlight-limited regimes like the Amazon . On the other hand, a reduction in low clouds over the ocean would make it more difficult to do marine cloud brightening at the same time as other forms of solar geoengineering. Changes in cirrus clouds are also relevant in the context of research on the effects of sedimentation of injected stratospheric aerosols on high clouds and proposals to intentionally thin cirrus clouds with nucleation-inducing aerosols in order to cool the Earth by increased LW emission . The increase in high clouds in most models in G1 indicates that thermodynamic and radiative adjustments to the forcing scenario can have effects on high clouds that may counteract unintentional or intentional microphysical effects. Our analysis of G1 also illustrates that stratospheric ozone could be affected by changes in stratospheric water vapor resulting from TTL temperature changes. In model runs with actual injection of sulfate aerosols, LW absorption of these particles warms the tropical tropopause and increases stratospheric water vapor, which results in decreased ozone concentrations . suggest that this risk could be mitigated by instead injecting calcite aerosols, which would absorb much less LW radiation than sulfates, but the inconsistency between models in stratospheric water vapor responses to the G1 experiment, which includes no aerosol injection in G1, shows that much uncertainty remains in this area. Taken together, these issues emphasize the importance of continuing to perform and analyze geoengineering simulations, both in highly idealized scenarios like G1 and more realistic ones like G4 or G4SSA , in order to better understand the climate responses to geoengineering schemes and the different roles played by thermodynamics, radiation, microphysics, and chemistry in these responses.

Code and data availability
Code and data availability.

All scripts used to analyze data and create plots are available at https://zenodo.org/record/1328272 (Russotto2018).

Supplement
Supplement.

Author contributions
Author contributions.

RDR analyzed the GCM output, produced the figures, and wrote the bulk of the paper. TPA provided general guidance and assisted with the preparation of the manuscript.

Competing interests
Competing interests.

The authors declare that they have no conflict of interest.

Special issue statement
Special issue statement.

Acknowledgements
Acknowledgements.

Three anonymous reviewers provided constructive comments that helped to improve the paper. This work was supported by a grant to JISAO from the Fund for Innovative Climate and Energy Research. For their roles in producing, coordinating, and making available the CMIP5 and GeoMIP model output, we acknowledge the climate modeling groups (listed in Table 1 of this paper), the World Climate Research Programme's (WCRP) Working Group on Coupled Modelling (WGCM), and the Global Organization for Earth System Science Portals (GO-ESSP). We are grateful to Duoying Ji, Ben Kravitz, Helene Muri, Ulrike Niemeier, Stephen Phipps, and Jin-Ho Yoon for helping to provide access to GeoMIP output that was not available through online repositories; to Karen Shell for helping to explain how to use the radiative kernels; and to Eui-Seok Chung for providing numbers for the double-call instantaneous forcing plotted in . We thank Dargan Frierson, Blaž Gasparini, Cristian Proistosescu, Brian Rose, and Robert Wood for discussions and comments that helped to influence the paper.

Edited by: Ben Kravitz
Reviewed by: three anonymous referees

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