1 Introduction

According to theories of stellar evolution (see, for example, Reference NewkirkNewkirk (1980) for a comprehensive review), the Sun was initially much fainter than it is at the present time. The solar luminosity of 4.7 Ga BP was calculated to be about 71% of the present value, increasing almost linearly since then (Reference Endal and SchattenEndal and Schatten 1982). It would appear that a decrease of the present value of solar luminosity by 20 to 30% could initiate an ice age and result in a totally ice-covered Earth (cf., for example, Reference North, Cahalan and CoakleyNorth and others 1981).

However, the geological record has indicated that the recent climate is more glacial than the long-term average (cf. Reference Tarling and GribbinTarling 1978, Reference CrowleyCrowley 1983). This would imply that, during most of the Earth’s history, the mean surface temperature has been near or above the present value. It also suggests that the Earth must have resisted complete glaciation during its evolution, although widespread glaciations were evident even in early climate history (e.g. the Huronian glaciation ~2.3 Ga BP). To complicate the picture further, there seems to be a decrease in the Earth’s surface temperature over the past 3 Ga (Reference Knauth and EpsteinKnauth and Epstein 1976), inferred from the isotopic analysis of cherts. This contradiction between the time-dependent solar output and the mean surface temperature of the Earth has been termed the “faint young sun-climate paradox”.

In studying the problem, it is more convenient to refer to the term ‘global stability” (cf. Reference Lindzen and FarrellLindzen and Farrell 1977), defined as the percent decrease of the present solar constant S₀ so that a totally ice-covered Earth occurs. Thus, the global stability represents the ability for the Earth-atmosphere climate system to resist complete glaciation in the face of a significantly reduced S₀.

Past studies of the global stability have been limited to the use of the one-dimensional zonal energy balance (ZEB) models. Reference BudykoBudyko (1969) and Reference SellersSellers (1969) have indicated that the global stability is small, about 2%. Using different meridional dynamical heat-flux parameterizations. Reference NorthNorth (1975) and Reference Lindzen and FarrellLindzen and Farrell (1977) obtained values of about 4 and 7%, respectively; Lindzen and Farrell also computed a value of 17% with an ad hoc Hadley stability ledge. More recent models (Reference CoakleyCoakley 1979, Reference Warren and SchneiderWarren and Schneider 1979) with improved parameterizations for the outgoing infrared (IR) flux and solar albedo yielded a value of about 10%. Warren and Schneider have also shown that the difference in the IR flux and albedo parameterizations could yield different global stability, ranging from 3 to 21%. On the other hand, using a one-dimensional vertical radiative-convective (VRC) model with ice albedo-temperature feedback and more comprehensive radiation parameterizations, Reference Wang and StoneWang and Stone (1980) computed the global stability to be about 11 to 23%, depending on the treatment of clouds.

Hypotheses have been proposed to explain the faint young sun-climate paradox. Reference Sagan and MullenSagan and Mullen (1972) and Reference HartHart (1978) discussed the possibility of the atmospheric greenhouse effect, associated with the chemical evolution of the Earth-atmosphere system. However, Reference Owen, Cess and RamanathanOwen and others (1979), Reference Kuhn and AtreyaKuhn and Atreya (1979), and Reference KastingKasting (1982) have argued against the ammonia- and methane-based greenhouse scenarios, primarily because the importance of these trace gases was limited to a small fraction of the Earth’s history and thus only H₂O and CO₂ could be possible candidates. A review of other possible hypotheses can be found in the work of Reference Endal and SchattenEndal and Schatten (1982).

Here, we show that the-climate feedback mechanisms, especially the vertical and meridional dynamical heat fluxes and their interactions, could act to maintain a much more stable climate. In particular, we use a coupled high- and low-latitude radiative-dynamical (HLRD) model to demonstrate the strength of such a strong climate-stabilizing effect. However, it must be borne in mind that the uncertainty associated with the dynamical heat-flux parameterizations is large, especially when used in a drastically different (from the present) climate. Nevertheless, our purpose is to demonstrate the role of such a plausible climate-stabilizing mechanism.

Below, we will first describe the physical model which includes these feedbacks. The model results of the effect of dynamical heat-flux feedbacks on global stability win be presented in section 3. In section 4, we summarize our findings.

2 Model

The coupled HLRD model is constructed to compute the annual mean northern-hemispheric temperature distribution T(x,z) as a function of altitude z and latitude ϕ where X = sinϕ. The vertical and meridional temperature structure is determined from heat balance between radiation and dynamical heat fluxes.

We use high vertical resolution (similar to the VRC model) because, as shown in Wang and others (Reference Wang and Stone1980, Reference Wang, Rossow, Yao and Wolfson1981), the change in vertical distribution of atmospheric trace constituents and clouds could have an important radiative effect on model climate sensitivity. However, very low-latitudinal resolution is chosen: two latitude zones are considered, i.e. a low latitude (0 to 30°N) and a mid-to-high latitude (30 to 90°N). Note that the low-latitudinal resolution will limit the study to the effect of dynamical heat fluxes on climate sensitivity on an annual basis. By using a two-zone model, the spatial scales are sufficiently large for one to anticipate that forced variations will dominate over free variations (Reference LorenzLorenz 1979). In addition, we minimize the complex problem of parameterizing the oceanic heat flux in low latitudes. Furthermore, as noted by Reference North, Cahalan and CoakleyNorth and others (1981), a two-zone latitudinal resolution is necessary and sufficient for using a two-mode Legendre polynomial expansion of meteorological fields (see discussion below). The two-zone resolution also allows for the moist adiabatic adjustment in the tropical region as well as for the baroclinic adjustment in high latitudes, which is a very important feature of the model climate system.

To represent the annual mean northern-hemispheric distribution of solar radiation reaching the top of the atmosphere S(x) and the surface temperature T_s(x), we use a two-mode representation (Reference NorthNorth 1975):

(1)

(2)

where P₂(x) is the second-order Legendre polynomial, S the mean value of S(x) and S₂ = −0.477 (Reference North, Cahalan and CoakleyNorth and others 1981). The northern-hemispheric mean surface temperature T_s and the effective meridional temperature contrast T₂ are the primary unknowns of the model.

In the HLRD model, the solar radiation is based on Reference Lacis and HansenLacis and Hansen (1974) while the thermal radiation formulation has been described in detail by Reference WangWang (1983). Spectral radiative properties of clouds were included in both the solar and thermal radiation calculations.

We use the empirical expression derived by Reference Stone and MillerStone and Miller (1980) to relate the total meridional heat transport (MHT) to the meridional surface temperature gradient. Specifically, from their equations, we find the total meridional heat flux D

(3)

The vertical dynamical heat flux is simulated by convective adjustment (Reference Manabe and StricklerManabe and Strickler 1964). Following Reference Stone and CarlsonStone and Carlson (1979), the critical lapse rate is chosen to be the moist adiábate r_m for the equatorial zone and at the 30 to 90^°N zone it is constrained by both r_m and r_b (the critical value for baroclinic adjustment). Note that, implicitly, r_b depends on the low-1 atitude r_m through its dependence on the meridional temperature gradient.

The ice albedo-temperature parameterization is similar to the one used by Reference Wang and StoneWang and Stone (1980). In the HLRD model, it is necessary to parameterize the change of the zonal surface albedo as a function of the ice-line change, which in turn depends on the changes in the zonal temperature distribution, i.e. in the two-mode representation T_s and T₂. The high-latitude surface albedo α_SH can be calculated from the following expression:

(4)

Whenever the ice-line reaches the low-latitude box, its surface albedo α_SL is given by

(5)

For both cases, the sine of the ice-edge latitude x_s is determined by

(6)

In the above equations b (= 0.63) is the ice-covered surface albedo, and its value was chosen to be consistent with satellite observations (Reference CoakleyCoakley 1979). The constants a_H (= 0.230) and a_L (=0.0873) are, respectively, the high- and low-latitude box ice-free-surface albedos, evaluated by averaging over the ocean and land albedos. Following the usual procedure, the ice-edge position is associated with a specified isotherm T_i(= −9.6^°c).

We will first adjust the model climate by matching the present values of T_s, T₂, the planetary albedo, the outgoing thermal flux and the ice-cap size, a necessary tuning process to obtain the so-called control run, or the simulated present climate.

The most significant improvement of the present HLRD model (over the one-dimensional VRC model) is the ability to simulate the tropospheric lapse rate. It is particularly encouraging to note that the tropospheric lapse rates at 0 to 30 and 30 to 90°N are calculated to be 6.1 and 4.8 K km⁻¹, respectively, which are in good agreement with observed values of 6.1 and 5.1 K km⁻¹ at the respective latitude zones. This feature is of critical importance for studying the interactions between the vertical and meridional heat fluxes and their effect on global stability.

3 Results

To study the effect of dynamical heat fluxes and their feedbacks on global stability, we ran the model with and without these feedbacks. For example, fixed vertical heat transport (VHT) means the vertical dynamical heat flux is fixed to be that of the control case (present climate) during climate change. Note that fixed VHT is different from the commonly-used fixed critical lapse-rate treatment, which still allows the VHT feedback.

As it has been pointed out by several authors (e.g. Reference Cess and WronkaCess and Wronka 1979, Reference Warren and SchneiderWarren and Schneider 1979, Reference Endal and SchattenEndal and Schatten 1982) that the meridional heat transport parameterization has a crucial influence on the ice extent, we investigate the changes of the total (ocean and atmosphere) meridional heat flux and ice cover in response to the decreases in the solar constant.

For this purpose, starting from the present equilibrium climate (the control case), the model was run with gradually reduced (i.e. no large perturbations were applied to any equilibrium climate) solar constant values until a totally ice-covered Earth occurred. Such a quasistatic perturbation treatment was intended to allow the feedback mechanisms inherent in the climate system to act smoothly, and thus to eliminate (if any) possible spurious solutions (see Reference North, Cahalan and CoakleyNorth and others 1981).

Figure 1 shows the model-calculated ice-line position as a function of the solar constant change. In the ZEB models, an unstable equilibrium state can be calculated (defined by dx_s/d(S/S₀) < 0). However, in the HLRD model, the corresponding unstable state cannot be reached because of the use of a time-marching procedure. Consequently, the results of the unstable transitions from our model are indicated by vertical lines.

Fig. 1 Feedback effects of meridional and vertical heat transport (MHT and VHT, respectively) on the ice-line position for solar constant change. Four scenarios were studied: fixed VHT, fixed both VHT and MHT, VHT and MHT feedbacks, and fixed MHT. The results for the former two scenarios are almost Identical and thus are represented by the same curve.

To study the dynamical heat-flux feedback, we have .performed four model calculations: fixed VHT (case 1), fixed both VHT and MHT (case 2), both VHT and MHT feedbacks (case 3) and fixed MHT (case 4). Note, however, that fixed dynamical heat transport scenarios are used only for illustrative purposes.

Because the results for cases 1 and 2 are almost identical, both are represented by the same curve in Figure 1. The calculated global stability for case 3 (considered to be the most realistic one of the four cases) is ~21%, which is in sharp contrast with the ~1% value obtained for cases 1 and 2. The results suggest that the vertical heat-flux feedback is a strong negative feedback during climate change. Case 4 (fixed MHT) reveals some interesting features. When the MHT feedback was switched off, other feedback mechanisms, for example, the lapse rate, interacted with each other in such a way that a 26% solar constant reduction was needed for a total freeze. Moreover, these solutions indicate that the Earth is ice-free for most of its history. Note that these results are also in sharp contrast with the calculations for case 3, in which the MHT feedback is included. In that case, the ice-cap exists even when the change of MHT is small (see Equation (3) and T₂ values in Table 1). The implication is that the model climate is very sensitive to the presence or absence of MHT feedback, in fact, the model’s current climate is unstable in the latter case. This kind of behavior for fixed MHT has been pointed out by Reference StoneStone (in press). In addition, Reference Barron, Thompson and SchneiderBarron and others (1981) have also found that if the present-day value of the meridional heat transport could be maintained (despite the decrease of the meridional temperature gradient) the nominally high Cretaceous temperatures (i.e. an ice-free Earth) can be achieved with a one-dimensional ZEB model.

Table I Effects of Treatments of Meridional Heat Transport (MHT) On Change of Model Climate Due to Solar Constant Decrease. In Both Treatments, The Vertical Heat-Transport Feedback is Included.

Table I presents comparisons between cases 3 and 4 of the changes of other model climate parameters. These comparisons show that the difference between the model behavior for the two cases can be attributed to the different responses of the vertical dynamical heat flux and the baroclinic lapse rate. The results also suggest that fixed MHT results in a significantly smaller meridional temperature gradient while for MHT feedback, T₂ maintains more or less a constant value, a feature also cited in Reference Wang and StoneWang and Stone (1980).

Another interesting point is that for both cases the tropopause height decreased when solar constant was reduced and reached ~400 to 500 mbar at the limiting value of global stability. Similar behavior was reported by Reference Wetherald and ManabeWetherald and Manabe (1975), who obtained a tropopause height of 500 mbar for their white Earth experiment. In our model simulations with MHT feedbacks, the oceanic fraction was assumed to be 50% of the total (the atmosphere contains the other 50%) before the ice line reaches 30°, and assumed zero thereafter (the atmosphere contains all the MHT). It was also found that keeping the ocean transport fixed (the same as the control experiment) led to a smaller global stability of ~18.5%.

4 Summary and Discussion

We have examined the faint young sun-climate paradox using a coupled high- and low-latitude radiative-dynamical model. The model computes solar and thermal radiation and, more importantly, considers meridional and vertical dynamical heat-flux feedbacks. The results indicate that by including these feedback mechanisms, the model climate becomes much more stable than previous model results have indicated. Therefore we argue that no deus ex machina assumptions are needed to explain the faint young sun-climate paradox. For example, an enormous amount of CO₂ is apparently not required to provide the greenhouse effect during the second half of the Earth’s history. This can be regarded as a very important consequence, since more recent findings (see Reference Endal and SchattenSchatten and Endal 1982, Reference CrowleyCrowley 1983 for details) point out that no great amounts of greenhouse gases were present during the last 2 Ga. The model results suggest that the climate feedback mechanisms alone, combined perhaps with moderately increased concentrations of greenhouse gases and/or lower surface albedos, as well as increased oceanic heat transport, could have maintained not just a higher global stability, but a relatively ice-free Earth on the geological time scales.

However, we must emphasize that since the dynamical heat-flux parameterizations were derived on a basis of the present climate conditions, they may not necessarily be valid when the climate is significantly different from that existing now. Moreover, the simple ice-edge conditions used for these experiments may be inadequate, especially when the ice line moves to low latitudes where the seasonal surface temperature variation is small.

In summary, much more work is needed in the context of global stability to develop more appropriate ice-line conditions, to parameterize oceanic heat transport and to construct surface albedo parameterization on geological time scales corresponding to the evolution of the lithosphere (Reference HargravesHargraves 1976). In addition, model improvements, such as interactive clouds, cumulus convective parameterization for the tropics and seasonal variation should also be pursued. These parameterizations together with an im-proved knowledge of the chemical evolution of the Earth’s atmosphere may bring us one step further to the understanding of the paradox.