## 1. Introduction

The growth rate of baroclinic instability waves has been widely used in the diagnosis of the storm-track activity. The growth rate of Eady baroclinic instability waves is proportional to the vertical wind shear and the inverse of the static stability of the basic state (Eady 1949). Lindzen and Farrell (1980) derived the growth rate of Charney waves in a form similar to that of Eady waves. Hoskins and Valdes (1990) showed the coincidence of the growth rate with the storm track in the Northern Hemispheric winter. Recently, many authors have tried to explain the global warming–induced change in storm track by means of the growth rate of Eady waves (e.g., Hall et al. 1994; Lunkeit et al. 1998; Geng and Sugi 2003; Yin 2005).

A question that has arisen is how the vertical profile of baroclinicity affects the wave activity. Global warming is projected to decrease the vertical wind shear in the lower troposphere but increase it in the upper troposphere and lower stratosphere (UTLS) (Solomon et al. 2007). The sea surface temperature gradients are important for baroclinic instability, as was mentioned by Lunkeit et al. (1998) in their simplified GCM. However, Yin (2005) stated in his multimodel ensemble analyses of the global warming that the poleward shift of the storm track is caused mainly by changes in the upper-tropospheric baroclinicity. The aquaplanet experiment by Kodama and Iwasaki (2009) showed that a polar SST rise reduces the baroclinic instability wave activity as expected, while a uniform SST rise enhances static stability in the subtropics and wind shear in the midlatitude upper troposphere and then shifts the storm track in the poleward direction.

The wave activity is understood in terms of energy conversion rates in the mass-weighted isentropic zonal means (MIM). MIM facilitates presenting Lagrangian-mean meridional circulations and wave–mean flow interactions (Gallimore and Johnson 1981; Andrews 1983; Townsend and Johnson 1985; Tung 1986; Iwasaki 1989) and exactly treats intersections of isentropes with the lower boundary, which is essential to the baroclinic instability (Iwasaki 1990). The basic part of the diagnosis package is available online (at http://wind.gp.tohoku.ac.jp/mim/).

MIM leads us to a simple cascade-type energy conversion diagram (Iwasaki 2001; Uno and Iwasaki 2006). The wave energy is generated from the zonal mean kinetic energy through the wave–mean flow interactions. In this work, the growth rate for instability wave is generalized, where the energy conversion rate need to be integrated over the certain domain. At first, it applies to Eady waves as a lesson for a conceptual understanding of the relationship between the energy conversion and the growth rate. Actual baroclinic instability waves are studied using aquaplanet simulation experiments. In particular, solar conditions are modified to study the sensitivity of wave activity to the UTLS vertical shear.

## 2. Generalized growth rate of baroclinic instability waves

*A*(

*x*,

*y*,

*θ*,

*t*) ≡

*A*(

*x*,

*y*,

*θ*,

_{S}*t*) are taken when

*θ*<

*θ*(

_{s}*x*). Isentropic zonal mean pressure is used for vertical coordinates

*p*

_{†}coordinates. The use of

*p*

_{†}coordinates makes it easy to consider the compatibility with the transformed Eulerian mean (TEM) diagnosis by Andrews and McIntyre (1976), except for the lower boundary condition. In both isentropic coordinates and

*p*

_{†}coordinates, the essential features of MIM come from the following definitions of zonal means:

*p*/∂

*p*

_{†}). The mass weight becomes zero when

*θ*<

*θ*(

_{s}*x*). Eddies are defined as

*A*and eddy kinetic energy

_{E}*K*:

_{E}*A*and

_{E}*K*in MIM are found in appendix A. The zonal mean system can easily separate the wave energy from the basic zonal mean state energy and diagnose the dynamic wave energy generation rate in the context of wave–zonal mean interactions. According to Iwasaki (2001) and Uno and Iwasaki (2006), globally integrated energy equations can be derived for the zonal mean available potential energy

_{E}*A*, zonal mean kinetic energy

_{Z}*K*, and wave energy:

_{Z}*Q*and

_{Z}*Q*are diabatic generation rates of the zonal mean and eddy available potential energies, respectively, and

_{E}*δ*and

_{Z}*δ*are the zonal mean and eddy dissipations, respectively. The definitions of parameters are shown in appendix D. In appendix A, we derive an important relationship of conversion rates,

_{E}*u*,

*υ*,

*ρ*

_{0}, Φ, Φ

_{†}, and

**F**are the zonal flow, meridional flow, reference density, geopotential height, geopotential height for the zonal ground state, and E-P flux, respectively. Here, the log pressure coordinate is defined as

*z*

_{†}≡ −

*H*log

*p*

_{†}/

*p*

_{0}. In

*C*(

*A*,

_{Z}*K*), the mean-meridional direct circulations convert the zonal mean available potential energy into the zonal mean kinetic energy. In

_{Z}*C*(

*K*,

_{Z}*W*), the zonal wave–mean flow interactions convert the zonal mean kinetic energy into the wave energy. In general, since the E-P flux exchanges negligibly small angular momentum with the solid earth, it mainly redistributes the angular momentum in the atmosphere while conserving its total value (Tanaka et al. 2004). Equation (11) indicates that the zonal mean kinetic energy is converted into the wave energy, when the E-P flux reduces the spatial variance of the mean zonal flow. Equation (12) is the local dynamic wave energy generation rate. The first and second terms are the shear production of wave energy and its vertical relocation, respectively. Spatial distributions of

*C*(

*K*,

_{Z}*W*) in a meridional plane are considerably different from those of

*C*(

^{W}*K*,

_{Z}*W*), although their global integrals are exactly equal as mentioned above. Waves are generated in a different place from where the zonal mean kinetic energy is lost through wave–mean flow interactions. Detailed discussions regarding local conversion rates are provided in section 5. In Eqs. (11) and (12),

*ϵv*and

*ϵv*′ are the energy conversion terms that are associated with mean meridional flow, and they are much smaller than the energy conversion terms of the zonal wave–mean flow interactions.

*C*(

^{W}*K*,

_{Z}*W*)〉/〈

*W*〉 if we neglect diabatic effects and dissipative processes. Thus, growth rate of instability waves can be generalized as

*C*(

*K*,

_{Z}*W*) is the sink of zonal mean kinetic energy, which is converted into the wave energy. This expression is convenient for discussing the wave energy source. The energy conversion rate is proportional to the mean zonal wind difference between the E-P flux convergence and divergence areas.

## 3. Energetics of Eady waves

Let us first consider the Eady problem (Eady 1949) to understand the essence of the baroclinic instability in the context of wave–mean flow interactions. MIM enables us to explicitly express the E-P flux divergence/conversion and mean-meridional flow in the Eady waves, both of which are caused by intersections of isentropes with lower/upper boundaries (Iwasaki 1990). The generalized growth rate defined above is obtained for Eady waves and compared with its conventional value.

*C*(

*A*,

_{Z}*K*) in compensation for the loss of zonal mean kinetic energy through

_{Z}*C*(

*K*,

_{Z}*W*). (d) The Coriolis force for mean-meridional flow accelerates (decelerates) the mean zonal flow near the upper (lower) boundary. It recovers the geostrophic balance of the Coriolis forces of the mean zonal flow with the meridional pressure gradient. These four steps [(a)–(d)] proceed simultaneously and continuously.

Processes of wave–mean flow interactions of Eady waves. Vertical and horizontal axes indicate altitude and mean zonal flow, respectively. (a) Eady waves generate upward E-P flux. (b) The E-P flux divergence accelerates zonal flow near the lower boundary and the convergence decelerates it near the upper boundary. (c) Intersections of isentropes with boundaries cause mean equatorward flow near the lower boundary and mean poleward flow near the upper boundary. (d) The Coriolis forces of the mean meridional flow decelerate the zonal flow near the lower boundary and accelerate it near the upper boundary.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Processes of wave–mean flow interactions of Eady waves. Vertical and horizontal axes indicate altitude and mean zonal flow, respectively. (a) Eady waves generate upward E-P flux. (b) The E-P flux divergence accelerates zonal flow near the lower boundary and the convergence decelerates it near the upper boundary. (c) Intersections of isentropes with boundaries cause mean equatorward flow near the lower boundary and mean poleward flow near the upper boundary. (d) The Coriolis forces of the mean meridional flow decelerate the zonal flow near the lower boundary and accelerate it near the upper boundary.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Processes of wave–mean flow interactions of Eady waves. Vertical and horizontal axes indicate altitude and mean zonal flow, respectively. (a) Eady waves generate upward E-P flux. (b) The E-P flux divergence accelerates zonal flow near the lower boundary and the convergence decelerates it near the upper boundary. (c) Intersections of isentropes with boundaries cause mean equatorward flow near the lower boundary and mean poleward flow near the upper boundary. (d) The Coriolis forces of the mean meridional flow decelerate the zonal flow near the lower boundary and accelerate it near the upper boundary.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

In the isobaric zonal mean system, the eddy heat transport is essential for baroclinic instability and conducts mean-eddy energy conversions. On the other hand, in the MIM without any eddy heat flux, the mean meridional flows, which are bounded to the upper or lower boundaries, conduct meridional heat transport and the energy conversion from the zonal mean available potential energy to the zonal mean kinetic energy.

*C*(

*K*,

_{Z}*W*) can be approximated by the following formula:

*U*and

_{T}*U*are basic zonal velocities at the top and bottom of the domain,

_{B}*F*is the vertical E-P flux in the free atmosphere, and

_{z}*L*is the meridional length. In appendix C, the vertical component of the E-P flux is derived as

_{y}*k*,

*c*, and

_{i}*λ*(≡

*U*−

_{T}*U*) are respectively the zonal wavenumber, imaginary phase velocity, and vertical shear per nondimensional vertical coordinates. Note that

_{B}*c*is the growth rate of the perturbation geopotential height of Eady waves. Substituting Eqs. (17) and (18) into Eq. (14), we have

_{i}k## 4. An aquaplanet experiment on the sensitivity to upper-level baroclinicity

As mentioned in the previous section, the intersections of isentropes with the lower (upper) boundaries play essential roles in the E-P flux divergence (convergence) and equatorward (poleward) mean flow in the Eady waves. In the actual atmosphere, the isentropes intersect the lower boundary as assumed in the Eady waves. However, the actual atmosphere does not have any rigid upper boundary, which is very different from the Eady waves. To see more realistic baroclinic instability waves, a diagnosis is made of an aquaplanet experiment for a perpetual equinox 10-yr simulation after a 1-yr spinup with a zonally symmetric sea surface temperature (Neale and Hoskins 2000). The model used is a Meteorological Research Institute (MRI)–Japan Meteorological Agency (JMA) global spectral model (GSM) (Shibata et al. 1999; Yukimoto et al. 2006). The model has a horizontal truncation wavenumber at triangular 63 and 45 vertical levels. The detailed setting of the control equinox experiment is found in Kodama and Iwasaki (2009).

Figure 3 shows vertical profiles of the vertical component of the E-P flux and its divergence at 45°N. The E-P flux has a maximum near 800 hPa and diverges (converges) below (above) this level. This is very different from Eady waves, whose E-P flux is vertically constant, except near the upper or lower boundaries. The leading term of the growth rate equation [Eq. (13)] is

Vertical profiles of (a) the vertical component of E-P flux (10^{5} kg s^{−2}) and (b) its divergence (m s^{−1} day^{−1}) at 45°N, averaged over 10 yr of the perpetual equinox experiment.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Vertical profiles of (a) the vertical component of E-P flux (10^{5} kg s^{−2}) and (b) its divergence (m s^{−1} day^{−1}) at 45°N, averaged over 10 yr of the perpetual equinox experiment.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Vertical profiles of (a) the vertical component of E-P flux (10^{5} kg s^{−2}) and (b) its divergence (m s^{−1} day^{−1}) at 45°N, averaged over 10 yr of the perpetual equinox experiment.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

The baroclinicity at single level, however, is not enough to estimate the growth rate in Eq. (13). In Eq. (14), 〈*C*(*K _{Z}*,

*W*)〉 is proportional to the zonal flow difference between the convergence and divergence areas. In this experiment, the convergence and divergence centers are located near 400 hPa and near 900 hPa, respectively, and their flow difference may cause the wave instability. How is the wave instability affected by the baroclinicity in the UTLS? A sensitivity experiment is designed to answer this question, where the solar condition is changed to the solstice without any change in the SST or zonal mean ozone distributions. Even though the SST is symmetric between the two hemispheres, the asymmetric solar heating due to ozone and water vapor makes a significant difference in the zonal mean temperature, particularly in the UTLS, as shown in Fig. 4. Thus, in midlatitudes, the UTLS meridional temperature gradient is much greater in the winter hemisphere than in the summer hemisphere. As a result, the UTLS vertical wind shear in midlatitudes is enhanced (reduced) in the winter (summer) hemisphere. It is somewhat strange that the subtropical jet stream is weakened (strengthened) in the winter (summer) hemisphere, in geostrophic balance with cooling (warming) in the subtropical upper troposphere of the summer (winter) hemisphere. This may result from the mismatch of the equinox SST under the solstice solar condition and be associated with eddy angular momentum transport (Held and Hou 1980). Such subtropical changes in the westerlies, however, seem to be smaller and to have much less impact on the baroclinic wave activity than the extratropical changes.

Meridional cross sections of (a) potential temperature [contour interval (CI) = 10 K], (c) zonal mean zonal flow (CI = 10 m s^{−1}), (e) E-P flux divided by pressure (vectors, kg s^{−2} Pa^{−1}), and its divergence (m s^{−1} day^{−1}), and (g) mass streamfunctions (CI = 5 × 10^{10} kg s^{−1} for 1000–100 hPa and 0.2 × 10^{10} kg s^{−1} for 100–10 hPa; negative values are shaded) averaged over the solstice run; and (b),(d),(f),(h) their deviations from the equinox run, where (b) has a CI = 2 K, (d) has a CI = 5 m s^{−1} (equinox run is shaded), (f) has units of kg s^{−2} Pa^{−1} (vectors), and m s^{−1} day^{−1}, and (h) has CIs = 1 × 10^{10} kg s^{−1} for 1000–100 hPa and 0.05 × 10^{10} kg s^{−1} for 100–10 hPa (negative values are shaded).

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Meridional cross sections of (a) potential temperature [contour interval (CI) = 10 K], (c) zonal mean zonal flow (CI = 10 m s^{−1}), (e) E-P flux divided by pressure (vectors, kg s^{−2} Pa^{−1}), and its divergence (m s^{−1} day^{−1}), and (g) mass streamfunctions (CI = 5 × 10^{10} kg s^{−1} for 1000–100 hPa and 0.2 × 10^{10} kg s^{−1} for 100–10 hPa; negative values are shaded) averaged over the solstice run; and (b),(d),(f),(h) their deviations from the equinox run, where (b) has a CI = 2 K, (d) has a CI = 5 m s^{−1} (equinox run is shaded), (f) has units of kg s^{−2} Pa^{−1} (vectors), and m s^{−1} day^{−1}, and (h) has CIs = 1 × 10^{10} kg s^{−1} for 1000–100 hPa and 0.05 × 10^{10} kg s^{−1} for 100–10 hPa (negative values are shaded).

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Meridional cross sections of (a) potential temperature [contour interval (CI) = 10 K], (c) zonal mean zonal flow (CI = 10 m s^{−1}), (e) E-P flux divided by pressure (vectors, kg s^{−2} Pa^{−1}), and its divergence (m s^{−1} day^{−1}), and (g) mass streamfunctions (CI = 5 × 10^{10} kg s^{−1} for 1000–100 hPa and 0.2 × 10^{10} kg s^{−1} for 100–10 hPa; negative values are shaded) averaged over the solstice run; and (b),(d),(f),(h) their deviations from the equinox run, where (b) has a CI = 2 K, (d) has a CI = 5 m s^{−1} (equinox run is shaded), (f) has units of kg s^{−2} Pa^{−1} (vectors), and m s^{−1} day^{−1}, and (h) has CIs = 1 × 10^{10} kg s^{−1} for 1000–100 hPa and 0.05 × 10^{10} kg s^{−1} for 100–10 hPa (negative values are shaded).

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Figure 5 shows the latitudinal profiles of the vertically integrated wave energy, *C ^{W}*(

*K*,

_{Z}*W*), and

*C*(

*K*,

_{Z}*W*). The solstice solar condition significantly enhances (reduces) the wave energy and its generation rate in midlatitudes of the winter (summer) hemisphere. The generalized growth rate is estimated from integrating the wave energy and its generation rate over each of hemispheres at about 0.065, 0.054, and 0.043 day

^{−1}for the solstice winter, equinox, and solstice summer, respectively. This is consistent with the fact that the integrated wave energy is greater in the winter hemisphere than in the summer hemisphere. Thus, the UTLS baroclinicity is considered to enhance the wave instability as well as the low-level baroclinicity. In this case, the generalized growth rate may indicate the statistical average of many waves over the hemisphere. Attention must be paid to the poleward (equatorward) shift of peak positions of wave energy and wave energy generation rates in the winter (summer) hemisphere under the solstice solar condition (Fig. 5). This problem will be discussed in the next section. The above estimate of the growth rate suggests that the wave energy generation rate must be a higher-order function of baroclinicity. In the analogy with the Eady waves, the E-P flux is expected to be proportional to wave energy. In reality, the E-P flux is greatly impacted by the change in solar condition, as shown in Fig. 4. Thus, the wave energy generation rate is expected to be of a higher order of baroclinicity than the wave energy, since it is the integration of inner product of E-P flux and shear vector of mean-zonal wind.

Meridional profiles of (a) vertically integrated wave energy, (b) wave energy generation rate, and (c) energy conversion rate averaged over the solstice experiment (Southern Hemispheric winter) with a weight of cos*ϕ*. The results of the equinox experiment are shaded.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Meridional profiles of (a) vertically integrated wave energy, (b) wave energy generation rate, and (c) energy conversion rate averaged over the solstice experiment (Southern Hemispheric winter) with a weight of cos*ϕ*. The results of the equinox experiment are shaded.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Meridional profiles of (a) vertically integrated wave energy, (b) wave energy generation rate, and (c) energy conversion rate averaged over the solstice experiment (Southern Hemispheric winter) with a weight of cos*ϕ*. The results of the equinox experiment are shaded.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

## 5. Local wave energy generation rates

Where is the wave energy generated from in the latitude–height section? Global warming has been projected to increase the upper-tropospheric eddy kinetic energy (Yin 2005). Similar changes were found in the aquaplanet experiment with a uniform SST rise (Kodama and Iwasaki 2009). In this section, discussions are extended to latitude–height distributions of the wave energy generation rate and its sensitivity to the vertical profile of baroclinicity in the above-mentioned aquaplanet experiment.

Figure 6 shows the meridional cross sections of wave energy, *C ^{W}*(

*K*,

_{Z}*W*), and

*C*(

*K*,

_{Z}*W*).

*C*(

^{W}*K*,

_{Z}*W*) has a temporal change term of geopotential height, which is the second term on the right-hand side of Eq. (12). This term is estimated from 3-hourly model outputs with the centered finite time difference. The wave energy has a local maximum in the midlatitude upper troposphere and increases along the polar night jet stream in the winter stratosphere. Roughly speaking, these overall meridional distributions of wave energy are similar to those of the wave energy generation rate, although the former is relatively greater than the latter in the stratosphere. Detailed differences between these distributions may come from the propagation, deformation, and dissipation of waves. The change in solar condition enhances (reduces) the wave energy generation rate and accordingly the wave energy in the midlatitude upper troposphere of the winter (summer) hemisphere. This is followed by the change in the wave energy, although the wave energy has relatively stronger impact in the stratosphere.

Meridional cross sections of (a) wave energy (CI = 50 J kg^{−1}), (c) wave energy generation rate (CI = 10^{−3} W kg^{−1}), and (e) energy conversion rate (CI = 10^{−3} W kg^{−1}) averaged over the solstice experiment, and (b),(d),(f) their deviations from averaging over the equinox with CI = (b) 20 J kg^{−1}, (d) 0.5 × 10^{−3} W kg^{−1}, and (f) 0.5 × 10^{−3} W kg^{−1}. Broken lines indicate negative contours.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Meridional cross sections of (a) wave energy (CI = 50 J kg^{−1}), (c) wave energy generation rate (CI = 10^{−3} W kg^{−1}), and (e) energy conversion rate (CI = 10^{−3} W kg^{−1}) averaged over the solstice experiment, and (b),(d),(f) their deviations from averaging over the equinox with CI = (b) 20 J kg^{−1}, (d) 0.5 × 10^{−3} W kg^{−1}, and (f) 0.5 × 10^{−3} W kg^{−1}. Broken lines indicate negative contours.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

Meridional cross sections of (a) wave energy (CI = 50 J kg^{−1}), (c) wave energy generation rate (CI = 10^{−3} W kg^{−1}), and (e) energy conversion rate (CI = 10^{−3} W kg^{−1}) averaged over the solstice experiment, and (b),(d),(f) their deviations from averaging over the equinox with CI = (b) 20 J kg^{−1}, (d) 0.5 × 10^{−3} W kg^{−1}, and (f) 0.5 × 10^{−3} W kg^{−1}. Broken lines indicate negative contours.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

_{0}exp[

*ik*(

*x*−

*ct*)], we have the relation

As in Fig. 6, but for (a) the meridional E-P flux term in *C ^{W}*(

*K*,

_{Z}*W*) (CI = 10

^{−3}W kg

^{−1}) and (c) the vertical E-P flux term, and (e) their sum; and (b),(d),(f) their respective deviations from averaging over the equinox with CI = 0.5 × 10

^{−3}W kg

^{−1}.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

As in Fig. 6, but for (a) the meridional E-P flux term in *C ^{W}*(

*K*,

_{Z}*W*) (CI = 10

^{−3}W kg

^{−1}) and (c) the vertical E-P flux term, and (e) their sum; and (b),(d),(f) their respective deviations from averaging over the equinox with CI = 0.5 × 10

^{−3}W kg

^{−1}.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

As in Fig. 6, but for (a) the meridional E-P flux term in *C ^{W}*(

*K*,

_{Z}*W*) (CI = 10

^{−3}W kg

^{−1}) and (c) the vertical E-P flux term, and (e) their sum; and (b),(d),(f) their respective deviations from averaging over the equinox with CI = 0.5 × 10

^{−3}W kg

^{−1}.

Citation: Journal of the Atmospheric Sciences 68, 4; 10.1175/2010JAS3609.1

*C*(

^{W}*K*,

_{Z}*W*) and

*C*(

*K*,

_{Z}*W*) (dynamic loss of zonal mean kinetic energy) is now further discussed. Equation (21) can be rewritten as

*C*(

^{W}*K*,

_{Z}*W*) adds two displacement terms to

*C*(

*K*,

_{Z}*W*) on the right-hand side of Eq. (22). Vertically integrated

*C*(

*K*,

_{Z}*W*) has double maxima in the subtropics and midlatitudes, as shown in Fig. 5. The subtropical maximum is largely caused by the meridional convergence of E-P flux. Possibly, waves propagating in the direction of the downgradient of mean zonal flow are absorbed by the mean flow near their critical latitudes

Finally, some comments are added with regard to the difference in the spatial distributions between *C ^{W}*(

*K*,

_{Z}*W*) and

*C*(

*K*,

_{Z}*W*). This is partly related to the invariance for the Galilean transformation of any constant zonal velocity. The zonal mean kinetic energy is not invariant for the Galilean transformation, so that

*C*(

*K*,

_{Z}*W*) is not invariant. On the other hand, the wave energy is invariant for the Galilean transformation. Equation (12) shows that all the terms of

*C*(

^{W}*K*,

_{Z}*W*) are invariant for the transformation. In particular, the temporal term

## 6. Conclusions

The baroclinic instability wave activity was studied in terms of wave–mean flow interactions, with a focus on the sensitivity to vertical profile of baroclinicity. The growth rate can be generalized as *α* ≡ 0.5〈*C ^{W}*(

*K*,

_{Z}*W*)〉/〈

*W*〉 = 0.5〈

*C*(

*K*,

_{Z}*W*)〉/〈

*W*〉, where the wave energy and its generation rate must be integrated over a certain domain. The zonal mean kinetic energy is reduced through the redistribution of zonal momentum due to the E-P flux divergence/convergence; accordingly, the reduced kinetic energy is converted into wave energy.

In the Eady waves, the generalized growth rate becomes consistent with the conventional value of baroclinic instability. The E-P flux is vertically constant except that its divergence and convergence are caused by intersections of isentropes with the lower and upper boundaries. The energy conversion rate from the zonal mean kinetic energy to the wave energy is proportional to the difference in mean zonal flow between upper and lower boundaries. This means that the vertical shear at each level evenly contributes to the instability. The mean-meridional flow caused by the intersections of isentropes with the upper and lower boundaries converts the zonal mean available potential energy into zonal mean kinetic energy in compensation for its loss due to wave energy generation.

Realistic baroclinic instability waves were studied by using aquaplanet experiments. The vertical component of the E-P flux is shown to have a maximum near 800 hPa, in contrast to the vertical constancy of the E-P flux in the Eady waves. The wave energy generation rate may be most sensitive to the baroclinicity at the maximal level of the E-P flux. The sensitivity of the wave activity to the low-level baroclinicity was confirmed in the authors’ previous impact study of a polar SST rise on the wave activity in aquaplanet experiments (Kodama and Iwasaki 2009). The generalized growth rate, however, integrates the baroclinicity over the certain domain and probably has an impact from the spatial distribution of baroclinicity. In this study, our attention is focused on the sensitivity to the upper-tropospheric and lower-stratospheric (UTLS) baroclinicity, where only the solar condition is changed from the equinox to the solstice without changing the SST. The generalized growth rates are shown to be sensitive to upper-tropospheric baroclinicity and causes differences in the hemispheric integration of wave energy.

Local wave energy is considered according to the wave energy generation rate, rather than the growth rate. The winter solstice condition increases the wave energy generation rate due to the enhanced UTLS vertical shear and accordingly increases wave energy in the midlatitude UTLS. Actual baroclinic instability waves considerably accompany the equatorward E-P flux in the UTLS, which plays important roles in subtropics–extratropics interactions in the upper troposphere. The equatorward flux causes extinction of wave energy through the processes of downgradient propagation of mean zonal flow in the subtropical upper troposphere.

The above considerations on the sensitivity of wave instability to the spatial profile of baroclinicity have implications for climate change due to global warming. Climate models tend to reduce the low-level baroclinicity but enhance the UTLS baroclinicity. These two changes are expected to have opposite effects on baroclinic wave activity. However, the relative magnitude of these two changes is dependent on the models. Their combined effects on the instability are so complicated that models may give a diversity of future projections for baroclinic wave activity.

## Acknowledgments

The atmospheric GCM used in this experiment was developed at the Meteorological Research Institute and the Numerical Prediction Division of the Japan Meteorological Agency. Parts of numerical experiments were performed at the Cyber-science Center, Tohoku University. This study is supported in part by the Japanese Ministry of Education, Culture, Sports, Science and Technology through a Grant-in-Aid for Scientific Research in Innovative Areas (2205).

## APPENDIX A

### Local Energy Conversion Rates

The authors’ previous works mainly focused on the globally integrated energies (Iwasaki 2001; Uno and Iwasaki 2006). This work deals with local energetics in latitude–height distributions, which is slightly complicated as compared with global integrals because the loss of the zonal mean kinetic energy *C*(*K _{Z}*,

*W*) has a different spatial distribution from that of the wave energy generation rate

*C*(

^{W}*K*,

_{Z}*W*). Here, the governing equations of local energetics are derived briefly.

*p*

_{†}and

*p*

_{††}, which are zonal and global means over isentropic surfaces, are used as the vertical coordinates for convenience. According to similar derivations, we have tendency equations of zonal and global ground-state potential energies as follows:

*A*(≡

_{Z}*P*−

_{Z}*P*) becomes

_{G}*A*is diabatically generated by meridional differential heating,

_{Z}*A*has three terms:

_{Z}*A*(≡

_{E}*P*−

*P*) as follows:

_{Z}*A*to

_{Z}*K*is conducted by the mean-meridional flow along the pressure gradient force as

_{Z}*A*in Eq. (A12), although their vertical distributions are different. Energy conversion from

_{Z}*K*to

_{Z}*W*is conducted by the deceleration of westerlies through wave–mean flow interactions as

*ϵv*are written as follows:

*ϵv*is the work due to the eddy forcing in the meridional direction; it is negligibly small as compared with that in the zonal direction.

*δ*is the frictional loss of the eddy kinetic energy. Uno and Iwasaki (2006) defined the wave energy as the eddy available potential energy and the eddy kinetic energy. Its tendency is given by

_{E}*C*(

^{W}*K*,

_{Z}*W*) is invariant for a Galilean transformation for any constant zonal velocity but the distribution of

*C*(

*K*,

_{Z}*W*) is not invariant, as discussed in section 5.

## APPENDIX B

### Local Wave Energy and Its Quasigeostrophic Expression

*p*(

*x*,

*θ*) −

*p*

_{†}≈ −[

*θ*(

*x*,

*p*=

*p*

_{†}) −

*θ*(

*p*

_{†})]∂

*θ*/∂

*p*

_{†}and

*N*

^{2}= (

*g*/

*θ*)(∂

*θ*/∂

*z*) = −(

*ρ*

_{0}

*g*

^{2}/

*θ*)(∂

*θ*/∂

*p*), it is approximated by isobaric zonal means as

## APPENDIX C

### Energy of Eady Waves

*z*≡ (

*p*−

_{s}*p*)/

*p*,

_{s}*U*(

*z*) ≡

*λz*+

*U*, and

_{B}## APPENDIX D

### List of Symbols

*u*, *υ* Zonal and meridional velocities

*T* Temperature

*θ* Potential temperature

*p* Pressure

Φ Geopotential height

**F** Eliassen–Palm flux

*t* Time

*x*, *y* East–west and north–south distances

*p*_{†}, *p*_{††} Isentropic zonal and global mean pressures

*z*_{†} Logarithmic pressure coordinates [≡−*H* log(*p*_{†}/*p*_{0})]

*w*_{†} Vertical velocity (≡*dz*_{†}/*dt*)

*ρ* Air density

*ρ*_{0} Reference air density [≡*p*_{†}/(*RT _{r}*)]

Φ_{†}, Φ_{††} Zonal and global ground-state geopotential heights (Φ_{†} ≡ ∫*RT*_{†} *d*ln*p*_{†}, Φ_{††} ≡ ∫*RT*_{††} *d*ln*p*_{††})

*A _{Z}*,

*A*Zonal mean and eddy available potential energies

_{E}*K _{Z}*,

*K*Zonal mean and eddy kinetic energies

_{E}*W* Wave energy

*C*(*A*, *B*) Energy conversion rate from *A* to *B*

*Q _{Z}*,

*Q*Generation rates of zonal mean and eddy available potential energies

_{E}*δ _{Z}*,

*δ*Dissipation rates of zonal mean and eddy kinetic energies

_{E}*ϵv*, *ϵv*′ Energy conversion *C*(*K _{Z}*,

*W*),

*C*(

^{W}*K*,

_{Z}*W*) associated with

*α* Growth rate of wave

*f* Coriolis parameter

*g* Gravitational constant

*R* Gas constant

*C _{υ}*,

*C*Heat capacities at constant volume and at constant pressure

_{p}Π Exner function [Π(*p*) ≡ *C _{p}p^{κ}p_{o}*

^{−κ}]

*p*_{0} Reference pressure

*κ* ≡*R*/*C _{p}*

*N* Brunt–Väisälä frequency

*U*, *U _{T}*,

*U*Zonal mean flow at each level, top level, and bottom level in Eady problem

_{B}*λ* Vertical shear of the Eady problem (≡*U _{T}* −

*U*)

_{B}*c _{i}* Imaginary phase speed of the Eady wave

*k* Zonal wave number of the Eady wave

*μ* Vertical exponent of the Eady wave

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