## 1. Introduction

The Madden–Julian oscillation (MJO) is the dominant component of intraseasonal (≈30–60 days) variability in the tropics (Madden and Julian 1971, 1972, 1994). It is an equatorial wave envelope of complex multiscale convective processes, coupled with planetary-scale (≈10 000–40 000 km) circulation anomalies. Individual MJO events often begin with a standing wave in the Indian Ocean, followed by eastward propagation across the western Pacific Ocean at a speed of roughly 5 m s^{−1} (Zhang 2005). In addition to its significance in its own right, the MJO also significantly affects many other components of the atmosphere–ocean–earth system, such as monsoon development, intraseasonal predictability in midlatitudes, and the development of the El Niño–Southern Oscillation (ENSO; Lau and Waliser 2005; Zhang 2005).

Despite the widespread importance of the MJO, present-day computer general circulation models (GCMs) typically have poor representations of it (Lin et al. 2006; Kim et al. 2009). Moreover, simple theories for the MJO have also been largely unsuccessful, both in explaining the MJO’s fundamental mechanisms and in reproducing all of its fundamental features together. There have been a large number of theories attempting to explain the MJO through mechanisms such as evaporation–wind feedback (Emanuel 1987; Neelin et al. 1987), boundary layer frictional convergence instability (Wang and Rui 1990), stochastic linearized convection (Salby et al. 1994), radiation instability (Raymond 2001), and the planetary-scale linear response to moving heat sources (Chao 1987). These theories are all at odds with the observational record in various crucial ways (Lau and Waliser 2005; Zhang 2005), and it is therefore likely that none of them captures the fundamental physical mechanisms of the MJO. Nevertheless, they all provide some insight into the mechanisms of the MJO.

Besides traditional GCMs and simple theories, further insight on the MJO has also been gained through other theoretical and modeling studies. For instance, insight has been gained from the study of MJO-like waves in multicloud model simulations (Khouider and Majda 2007; Majda et al. 2007; Khouider and Majda 2008b; Khouider et al. 2011) and in superparameterization computer simulations (Grabowski 2001, 2003; Grabowski and Moncrieff 2004; Moncrieff 2004; Benedict and Randall 2009; Thayer-Calder and Randall 2009), which appear to capture many of the observed features of the MJO by accounting for smaller-scale convective structures within the MJO envelope. As another example, convective momentum transport from subplanetary-scale waves/convection appears to play a role in producing some features of the MJO’s planetary-scale envelope, as shown in multiscale asymptotic models (Majda and Biello 2004; Biello and Majda 2005; Biello and Majda 2006; Biello et al. 2007; Majda and Stechmann 2009a). Despite all of the interesting contributions listed above—from GCMs, simplified models, and everything in between—no theory for the MJO has yet been generally accepted, and the problem of explaining the MJO has been called the search for the Holy Grail of tropical atmospheric dynamics (Raymond 2001). Building on earlier work, the present paper contributes to this search.

While theory and simulation of the MJO remain difficult challenges, they are guided by the generally accepted, fundamental features of the MJO on intraseasonal–planetary scales. These features are referred to here as the MJO’s “skeleton” (Majda and Stechmann 2009b), and they have been identified relatively clearly in observations:

- A slow eastward phase speed of roughly 5 m s
^{−1}(Hendon and Salby 1994; Hendon and Liebmann 1994; Maloney and Hartmann 1998; Kiladis et al. 2005), - A peculiar dispersion relation with
*dω*/*dk*≈ 0 (Salby and Hendon 1994; Wheeler and Kiladis 1999; Roundy and Frank 2004), and - A horizontal quadrupole vortex structure (Hendon and Salby 1994; Hendon and Liebmann 1994; Maloney and Hartmann 1998).

Recently, Majda and Stechmann (2009b) introduced a minimal dynamical model that captures the MJO’s intraseasonal/planetary-scale features 1–3, together, for the first time in a simple model. The model is a nonlinear oscillator model for the MJO skeleton and the skeleton of tropical intraseasonal variability in general. The fundamental mechanism of the model involves interactions between (i) planetary-scale, lower-tropospheric moisture anomalies and (ii) subplanetary-scale, convection/wave activity (or, more precisely, the planetary-scale envelope of the subplanetary-scale convective activity).

While the linear waves of the skeleton model were analyzed in Majda and Stechmann (2009b), the purpose of the present paper is to study the model’s nonlinear dynamics. Do the nonlinear dynamics also reproduce a realistic MJO skeleton? In what ways do the linear waves interact nonlinearly? In what ways do the waves interact nonlinearly with a regionally varying base state, which represents the western Pacific warm pool? When the warm pool is present, does the MJO skeleton often begin as a standing wave and then propagate slowly eastward? These questions and others are the focus of this paper.

The paper is organized as follows. In section 2, the model, its energetics, and its linear waves are described. Next, nonlinear numerical solutions are presented with a uniform base state [i.e., sea surface temperature (SST)] (section 3) and with a regionally varying, warm-pool SST (section 4). Finally, section 5 presents the conclusions.

## 2. Model description, energetics, and linear theory

### a. Model description

The MJO skeleton model was originally proposed and developed by Majda and Stechmann (2009b). It is a nonlinear oscillator model for the MJO skeleton as a neutrally stable wave (i.e., the model includes neither damping nor instability mechanisms). The fundamental mechanism of the oscillation involves interactions between (i) planetary-scale, lower-tropospheric moisture anomalies and (ii) subplanetary-scale, convection/wave activity (or, more precisely, the planetary-scale envelope of the subplanetary-scale convective activity). These quantities are represented by the variables *q* and *a*:

*q*: Lower-tropospheric moisture anomaly.*a*: Amplitude of the convection/wave activity envelope.

*q*–

*a*interaction is how the moisture anomalies influence the convection. The premise is that, for convective activity on planetary/intraseasonal scales, it is the time tendency of convective activity—not the convective activity itself—that is most directly related to the (lower tropospheric) moisture anomaly. In other words, rather than a functional relationship

*a*=

*a*(

*q*), it is posited that

*q*mainly influences the tendency (i.e., the growth and decay rates) of the convective activity. The simplest equation that embodies this idea iswhere Γ is a constant of proportionality: positive (negative) low-level moisture anomalies create a tendency to enhance (decrease) the envelope of convection/wave activity.

The basis for (1), and the physics behind it, comes from a combination of observations, modeling, and theory. Generally speaking, it is well-known that tropospheric moisture content plays a key role in regulating convection (Austin 1948; Malkus 1954; Brown and Zhang 1997; Tompkins 2001; Derbyshire et al. 2004; Grabowski and Moncrieff 2004; Holloway and Neelin 2009; Waite and Khouider 2010). In observations, specifically on planetary/intraseasonal scales, several studies have shown that the lower troposphere tends to moisten during the suppressed convection phase of the MJO, and lower-tropospheric moisture leads the MJO’s heating anomaly (Myers and Waliser 2003; Kikuchi and Takayabu 2004; Kiladis et al. 2005; Tian et al. 2006), which suggests the relationship in (1). Furthermore, this relationship is also suggested by simplified models for synoptic-scale convectively coupled waves (Khouider and Majda 2006; Khouider and Majda 2008a; Majda and Stechmann 2009a; Stechmann et al. 2011, manuscript submitted to *Theor. Comput. Fluid Dyn.*, hereafter SMS). These models show that the growth rates of the convectively coupled waves depend on the wave’s environment, such as the environmental moisture content; and SMS estimate the value of Γ from these growth rate variations. Last, amplitude equations such as in (1) have been used in other areas of science and engineering, and they can sometimes be derived from the governing equations using systematic asymptotics [see Bourlioux and Majda (1995) and references therein]. In the atmospheric sciences, SMS show that amplitude equations can be used as a simple model for convectively coupled wave–mean flow interactions (Majda and Stechmann 2009a).

*u*,

*υ*, and

*w*are the zonal, meridional, and vertical velocity anomalies, respectively;

*p*and

*θ*are the pressure and potential temperature anomalies, respectively; and

*s*and

^{θ}*s*are sources of cooling and moistening, respectively. The convective heating and drying are taken to be proportional to the envelope of convection/wave activity

^{q}Notice that this model contains a minimal number of parameters, summarized in Table 1: ^{−1} day^{−1} in dimensional units. These will be the parameter values used throughout the paper. The source terms *s ^{θ}* and

*s*must also be specified (see below). Also notice that the parameter

^{q}*a*); it is written here for clarity of presentation: dimensionally, it gives

*a*nondimensional. The dimensional value of

^{−1}so that a typical value of

*a*is ≈0.1, similar to the nondimensional value of

*u*.

Model parameters. The additional parameter ^{−1}.

*q*and

*a*:Next, for the meridional truncation, it is assumed that

*a*, the envelope of convection/wave activity, has a simple equatorial meridional structure proportional to

*K*and

*R*are the amplitudes of the Kelvin and equatorial Rossby structures, respectively, as shown in Fig. 1.

An important point is that *K*(*x*, *t*) and *R*(*x*, *t*) are the amplitudes of the structures of Kelvin and Rossby waves, but these amplitudes in (4) need not always propagate like “dry” waves. In the absence of forcing in (4), the dry long-wave Kelvin and equatorial Rossby wave solutions are dispersionless waves that propagate at 50 and 17 m s^{−1}, respectively (Majda 2003; Biello and Majda 2006). However, in the presence of the coupled dynamical forcing *A* in (4), the Kelvin and equatorial Rossby wave structures can be coupled to each other and to *Q* and *A*; and these coupled modes/structures can have propagation speeds very different from 50 or 17 m s^{−1}, and they can be dispersive. One such mode has the structure and dispersion characteristics of the MJO, as shown by Majda and Stechmann (2009b) and summarized below.

*u*,

*υ*,

*θ*are recovered by using the following formulas (Majda 2003; Biello and Majda 2006):where

*ϕ*

_{0}(

*y*) =

*π*

^{−}^{1/4}exp(−

*y*

^{2}/2),

*ϕ*

_{2}(

*y*) =

*π*

^{−}^{1/4}2

^{−}^{1/2}(2

*y*

^{2}− 1) exp(−

*y*

^{2}/2) are parabolic cylinder functions (Majda 2003; Biello and Majda 2006). The meridional structures of

*q*and the source terms are given by

*q*(

*x*,

*y*,

*t*) =

*Q*(

*x*,

*t*)

*ϕ*

_{0}(

*y*),

*s*(

^{θ}*x*,

*y*) =

*S*(

^{θ}*x*)

*ϕ*

_{0}(

*y*), and

*s*(

^{q}*x*,

*y*) =

*S*(

^{q}*x*)

*ϕ*

_{0}(

*y*). In the simplest case,

^{−1}is the uniform radiative cooling rate. Also notice that

*A*(

*x*,

*t*) is an anomaly from a base state

### b. Energetics

*s*and

^{θ}*s*. First, the model in (3) conserves a vertically integrated moist static energy:Second, the model in (3) conserves a positive total energy that includes a contribution from the convective activity

^{q}*a*:This total energy is a sum of four terms: dry kinetic energy

*u*

^{2}/2, dry potential energy

*θ*

^{2}/2, a moist potential energy proportional to

### c. Linear theory

^{−1}(Fig. 2a), an oscillation frequency that is roughly constant (Fig. 2e), and a horizontal quadrupole vortex structure (Fig. 2b). Furthermore, the nearly constant oscillation frequency is given by the following simple formula (Majda and Stechmann 2009b):On the other hand, the westward-propagating moist Rossby mode has a very low frequency that is essentially seasonal, not intraseasonal, for

*k*= 1. Previously, the

*k*= 1 and 2 moist Rossby modes were shown to have much smaller components of moisture

*Q*and convective activity

*A*in comparison to the MJO mode (Majda and Stechmann 2009b).

Here, in Fig. 2, emphasis is instead given to the *k* = 3, 4, and 5 moist Rossby modes because observational analyses often show a spectral peak at these wavenumbers and at intraseasonal frequencies (periods of greater than roughly 25 days; Wheeler and Kiladis 1999; Roundy and Frank 2004; Kiladis et al. 2009). The observed peak appears within a broader spectral band, which includes higher frequencies and greater wavenumbers, and that is associated with convectively coupled equatorial Rossby waves. It is possible that some aspects of the low-frequency Rossby wave activity are represented in the present model, although a detailed comparison of this is not the focus here. With this in mind, the model’s westward-propagating low-frequency mode is referred to here as the moist Rossby mode or wave, for simplicity. In addition to the two low-frequency modes of the model shown in Fig. 2, two high-frequency modes are also present; they resemble the dry Kelvin and Rossby waves and have little contribution from moisture or convective activity.

While the model in (2)–(4) adds little complexity beyond the dry primitive equations, one might suspect that the MJO skeleton could be captured by an even simpler version of (2)–(4). In light of this, a simpler version is briefly described now, including its strengths and limitations. To create a simpler version, the dry dynamics in (2)–(4) could be replaced by weak-temperature-gradient dynamics (Sobel et al. 2001; Majda and Klein 2003). A nice result of this approximation is that the oscillation frequency of the low-frequency waves is given exactly by (8) (see the appendix for details). However, it is not clear that this weak-temperature-gradient approximation is valid on intraseasonal/planetary scales (Majda and Klein 2003), and, more importantly, the dynamics loses its east–west asymmetry (i.e., both the eastward- and westward-propagating low-frequency modes have the same oscillation frequencies, in contrast to the results in Fig. 2).

### d. Numerical methods for the nonlinear model

The remainder of the paper describes nonlinear numerical solutions of the MJO skeleton model. The numerical method used to solve (4) is a splitting method that is designed to minimize numerical dissipation. In the first step, the linear equations for *K*, *R*, and *Q* are solved with the linearized part of the *A* equation: *K*, *R*, and *Q* are held fixed, and the nonlinear part of the *A* equation is evolved as a linear ordinary differential equation: *A _{t}* = Γ

*QA*. Each step is individually solved exactly: the first step using Fourier series, and the second step using the exact exponential solution (assuming

*Q*is held fixed). The initial condition for each case is either a single linear mode or a linear combination of two linear modes, as described below and summarized in Table 2. The initial amplitude is ≈0.1 in nondimensional units, which corresponds to a convective heating anomaly

^{−1}and a zonal wind anomaly of ≈±4 m s

^{−1}. Note that this is nearly the largest possible amplitude for a sinusoidal anomaly because

^{−1}. The spatial grid has 64 zonal grid points over the 40 000-km circumference of the earth, which yields a grid spacing of Δ

*x*= 625 km. This grid spacing allows each planetary wavenumber 1 to ≈6 to be resolved by at least 10 grid points. The time step was chosen to be Δ

*t*= 0.5Δ

*x*in nondimensional units, or Δ

*t*≈ 1.7 h. The data snapshots were output twice daily. A key feature of this model is that it is very inexpensive computationally: 1600 days of simulation time takes only ≈20 s of computer time on a typical laptop computer.

Summary of numerical experiments.

## 3. Nonlinear dynamics

In this section, nonlinear numerical solutions are presented with a uniform SST, as represented by the uniform base-state balance ^{−1}. The cases are summarized in Table 2.

### a. Case U2: Initial wavenumber-2 MJO

The simplest case is case U2 with uniform SST and an initial wavenumber-2 MJO mode. The results are shown in Fig. 3. The broad evolution is shown by the evolution of the convective activity ^{−1}, with prominent phases of both active and suppressed convection. In this nonlinear case, the convective anomalies are asymmetric: the positive anomalies have strong fluctuations of ≈1–3 K day^{−1}, whereas the negative anomalies never fall below −1 K day^{−1} because ^{−1}. Further indication of nonlinear effects can be seen in the excitation of other types of waves: a slow, westward-propagating envelope of maximum convective activity can be seen in Fig. 3a, and fast, westward-propagating signals can be seen throughout Fig. 3b.

Snapshots of the zonal–vertical structure (Fig. 3c) and zonal–meridional structure (Figs. 3d,e) are shown at time *t* = 150 days. Two strong convective events are present at this time with each collocated with upward vertical motion and horizontal convergence of the zonal wind. Straddling the equator, a pair of anticyclones leads and a pair of cyclones trails the convective activity. Also, the maximum lower-tropospheric moisture leads the convective maximum. Hence, the nonlinear model reproduces the fundamental features of the MJO skeleton.

While the model captures the broad fundamental features of the MJO, some finer details of the MJO’s muscle are not included in this model. These details include, for instance, a refined vertical structure (Lin and Johnson 1996; Myers and Waliser 2003; Kikuchi and Takayabu 2004; Kiladis et al. 2005; Tian et al. 2006), upscale momentum transport from mesoscale convective systems and synoptic-scale convectively coupled equatorial waves (Moncrieff and Klinker 1997; Houze et al. 2000; Tung and Yanai 2002a,b; Majda and Biello 2004; Biello and Majda 2005; Majda and Stechmann 2009a), and the effect of variations in land–sea contrasts and surface fluxes (Sobel et al. 2008, 2010). These effects should amplify features such as the westerly wind burst, and they would also likely rectify some of the finer details of the phase relationships among different variables (although some phase relationships are somewhat rectified in the warm-pool case of section 4a).

### b. Case U12: Initial wavenumbers-1 and -2 MJO

Case U12 illustrates the nonlinear interaction of different MJO wavenumbers, using an initial condition that is the sum of wavenumber-1 and -2 MJO modes. Figure 4a shows the broad evolution of the convective activity for 1600 days. The MJO events are organized by a slow, wavenumber-1, eastward-propagating envelope, whose existence is due to linear, not nonlinear, dynamics. Within this envelope, however, the individual MJO events have a variety of amplitudes and other nonlinear features that distinguish this case from purely linear dynamics. For instance, in this model simulation, it is common to see a strong MJO event followed by a weaker event (or vice versa), as was seen during the Tropical Ocean and Global Atmosphere Coupled Ocean–Atmosphere Response Experiment (TOGA COARE; Lin and Johnson 1996; Yanai et al. 2000). This is shown in greater detail in Fig. 4b; for example, near *x* ≈ 10 000 km, strong events at roughly *t* = 20 and 250 days are followed by weaker events at roughly *t* = 50 and 290 days, respectively.

### c. Case U13: Initial wavenumbers-1 and -3 MJO

The final case with uniform SST is case U13, shown in Fig. 5. To illustrate which features are nonlinear and which are linear, case U13 is shown in Figs. 5a,b and the linear version of case U13 is shown in Figs. 5c,d. This figure shows that a wavenumber-2 envelope of MJO events arises in both the nonlinear and linear versions, and its existence is due to linear dynamics. Within this envelope, the linear version displays identical MJO events with equal positive and negative amplitudes. On the other hand, the nonlinear dynamics creates a variety of different MJO events with long or short lifetimes, strong or weak amplitudes, stronger positive anomalies than negative anomalies, etc. For instance, in the time period from *t* = 150 to 250 days, there are strong MJOs with positive anomalies above 1 K day^{−1} between *x* = 0 and 10 000 km, and, at the same time, there are weaker MJOs with amplitudes below 1 K day^{−1} between *x* = 20 000 and 30 000 km.

## 4. Nonlinear dynamics with regional variations

While the previous section illustrated nonlinear dynamics with a uniform SST, this section illustrates the effect of an SST with warm-pool regional variations. The variations in the background state *x* ≈ 10 000 to 30 000 km and a cold pool elsewhere.

### a. Case WP-MJO: Initial MJO

In case WP-MJO, a warm-pool base state is used with a wavenumber-2 MJO as the initial condition. The long-term evolution of the convective activity is shown in Fig. 7. After an initial adjustment period, the convective activity aligns itself over the warm pool from roughly time *t* ≈ 2000 days and thereafter. The MJO events have prominent phases of both active and suppressed convection, and each event has its own individual characteristics in terms of strength, lifetime, regional variations, etc. Furthermore, in addition to the prominent eastward-propagating disturbances, there are instances of localized standing oscillations throughout the domain. For instance, there are standing oscillations localized near *x* ≈ 11 000 km during the period from roughly *t* = 2300 to 2500 days, toward the western end of the warm pool. This is in broad agreement with the visual appearance of standing oscillations in the Indian Ocean, often at the beginning of an MJO event (Lau and Chan 1985; Zhang and Hendon 1997; Kiladis et al. 2005).

To further explore the standing oscillations, the data is projected onto the eastward- and westward-propagating eigenmodes, as shown in Fig. 8. The eigenmode data is obtained by projecting the data vector [*K*(*x*, *t*), *R*(*x*, *t*), *Q*(*x*, *t*), *A*(*x*, *t*)]^{T} onto the linear eigenmodes in Fourier space, for each wavenumber *k* and at each time *t*. The resulting data include the eigenmode anomalies *e*_{MJO}(*x*, *t*) and *e*_{mR}(*x*, *t*) of the MJO mode and the moist Rossby mode, respectively; and it should be kept in mind that these linear eigenmodes actually have nonlinear dynamics. The evolution of *e*_{MJO}(*x*, *t*) and *e*_{mR}(*x*, *t*) is shown in Figs. 8a,b, respectively, for the final 1600 days from Fig. 7; and the time-averaged root-mean-squares (rms) of the anomalies are shown in Figs. 8c,d, respectively. The MJO mode anomalies are, on average, roughly centered around *x* = 20 000 km, the location of the maximum SST anomaly. The moist Rossby anomalies have smaller amplitudes than the MJO anomalies; they are not as coherent and their rms is slightly larger in the western part of the warm pool than in the eastern part. This suggests that, in this model, standing oscillations may be slightly more common in the western part of the warm pool than in the eastern part. In some specific instances, standing oscillations from Fig. 7 can be identified in Fig. 8 as instances with anomalies in both *e*_{MJO} and *e*_{mR}; one example is the region localized near *x* ≈ 11 000 km during the period from roughly *t* = 2300 to 2500 days, toward the western end of the warm pool, which was mentioned in the previous paragraph. In the model results here, the visual appearance of standing oscillations—without overwhelming statistical evidence for them—is in accord with the observational analyses of Zhang and Hendon (1997). More instances of visual evidence are shown in the zoomed-in figures described next.

To illustrate the details of a few MJO events, the final 200 days from Fig. 7 are shown in detail in Fig. 9, along with plots of the other variables: *Q*(*x*, *t*), *K*(*x*, *t*), and *R*(*x*, *t*). Two rectangular boxes are drawn in Figs. 9a,b to identify instances of localized standing oscillations: *x* = 11 000–15 000 km, *t* = 3400–3470 days, and *x* = 15 000–19 000 km, *t* = 3440–3530 days. Localized standing oscillations are prominent again, later, in the region *x* = 15 000–19 000 km, *t* = 3550–3600 days (for comparison, no box added). These plots show the details of the significant variations in the MJO events, including their amplitudes, propagation, lifetimes, and/or regional extent.

Moreover, these plots also show significant dry wave activity, which is particularly clear in the plots of *K* and *R* in Figs. 9c,d. These plots each display two prominent signals: the MJO signal dominates the warm-pool region in both plots because the MJO includes significant contributions from both *K* and *R* structures (cf. Fig. 2), and dry Kelvin and equatorial Rossby waves dominate the cold-pool regions in Figs. 9c,d, respectively. These dry waves can also be seen in the warm-pool region, where they appear as fluctuations in the MJO signal in Figs. 9c,d; and the convergence from these dry waves strongly affects the moisture anomalies, as seen in Fig. 9b; but the signature of the dry waves does not stand out in the convective activity in Fig. 9a, even though they likely contribute to the fluctuations in convective activity indirectly, through the moisture anomalies. It is also interesting that the beginning and end of almost all MJO events appear concomitant with dry wave signals in the cold pool. This appears in four different ways in Figs. 9c,d: (i) Kelvin waves often impinge on the western side of the warm pool near *x* ≈ 15 000 km and appear to “trigger” the next MJO event, (ii) Kelvin waves often appear to be “ejected” into the cold pool when MJO events end near *x* ≈ 25 000 km, (iii) equatorial Rossby waves often impinge on the eastern side of the warm pool near *x* ≈ 25 000 km and appear to “terminate” an MJO event, and (iv) equatorial Rossby waves often appear to be ejected into the cold pool when MJO events start near *x* ≈ 15 000 km.

The series of snapshots in Fig. 10 shows the detailed evolution and horizontal structure of an individual MJO event. Four snapshots of *q*(*x*, *y*), and horizontal velocity are shown at 10-day intervals from *t* = 3480 to 3510 days. The MJO event begins as a localized standing oscillation between *x* ≈ 15 000 and 20 000 km, as can be seen in Fig. 9 and in the sign changes in *q* from Figs. 10a,b. The enhanced convection in Fig. 10b is at the center of a horizontal quadrupole vortex structure. Ten days later, the enhanced convection has propagated eastward to *x* ≈ 22 000 km, as shown in Fig. 10c, and it is flanked by significant regions of suppressed convection. Last, the final stage of the life cycle is seen in Fig. 10d, where the enhanced convection has reached the eastern extent of the warm pool near *x* ≈ 23 000–27 000 km, and a westerly wind burst is evident [although its strength is weak compared to observations because this model does not include any mechanisms of the MJO’s muscle, such as upscale convective momentum transport (Tung and Yanai 2002a,b; Moncrieff 2004; Majda and Biello 2004; Majda and Stechmann 2009a)].

Finally, notice that this nonlinear case demonstrates, to a degree, a rectification of some finer details of the phase relationships in the MJO skeleton, in comparison to linear theory. For instance, in the nonlinear dynamics, the enhanced convection is typically collocated with zonal convergence, as in linear theory; however, there are instances when enhanced convection is collocated with low-level westerlies, such as the final stages of the life cycle in Fig. 10d, at the eastern extent of the warm pool near *x* ≈ 24 000 km. As another example, in the nonlinear dynamics, enhanced convection is typically led by enhanced lower-tropospheric moisture, as in linear theory; however, there are instances when convection and lower-tropospheric moisture anomalies are collocated, such as the negative anomalies in the eastern part of the warm pool (*x* ≈ 25 000 km) in Fig. 10b and in the western part of the warm pool (*x* ≈ 17 000 km) in Fig. 10c. As mentioned before, even further rectification would be expected to occur from the effects of a refined vertical structure (Lin and Johnson 1996; Myers and Waliser 2003; Kikuchi and Takayabu 2004; Kiladis et al. 2005; Tian et al. 2006), upscale momentum transport from mesoscale convective systems and synoptic-scale convectively coupled equatorial waves (Moncrieff and Klinker 1997; Houze et al. 2000; Tung and Yanai 2002a,b; Majda and Biello 2004; Biello and Majda 2005; Majda and Stechmann 2009a), and the effect of land–sea contrasts and surface fluxes (Sobel et al. 2008, 2010). Overall, this case captures the broad fundamental features of the MJO skeleton, in a model with minimal complexity.

### b. Case WP-K: Initial Kelvin

Case WP-K is another case with a warm-pool base state, but the initial condition is a wavenumber-2 Kelvin wave. As shown in Fig. 11, both MJO and moist Rossby modes are excited initially. At later times, from roughly *t* = 100 to 200 days, the central and eastern parts of the warm pool are dominated by the eastward-propagating mode, whereas the far-western warm pool and the cold pool are dominated by the westward-propagating mode (or standing oscillations). This case demonstrates the excitation of the moist waves by an initial dry wave, and it shows, in a nonlinear context, that the eastward-propagating mode is favored in the warm pool over the westward-propagating mode. This latter point corroborates the linear theory results that also suggest that the eastward-propagating mode is more strongly coupled with convection and moisture (Majda and Stechmann 2009b).

### c. Case WP-MR: Initial moist Rossby

Finally, Case WP-MR has a warm-pool base state and an initial wavenumber-2 moist Rossby wave (not shown). In this case, the moist Rossby wave does not have its largest amplitudes over the warm pool, as the MJO did (cf. Fig. 7). Instead, the moist Rossby wave has nearly uniform amplitude throughout the domain, with a slightly higher amplitude over the cold pool. This further corroborates the nonlinear Case WP-K and the linear theory results from Majda and Stechmann (2009b) that also suggest that the westward-propagating mode is less strongly coupled with convection and moisture.

## 5. Conclusions

A minimal, nonlinear oscillator model was presented for the MJO skeleton. As introduced recently by Majda and Stechmann (2009b), the fundamental mechanism of the model involves interactions between (i) planetary-scale, lower-tropospheric moisture anomalies and (ii) the envelope of subplanetary-scale, convection/wave activity. The interactions are neutrally stable (i.e., damping and instabilities on planetary–intraseasonal scales are absent). Furthermore, the model conserves the total energy in (7), which includes a component from the convective activity. The linear and nonlinear waves have been shown to capture, together, the fundamental features 1–3 of the MJO skeleton. Whereas the linear waves were analyzed by Majda and Stechmann (2009b) and summarized here in Fig. 2, the main focus of this paper is the model’s nonlinear dynamics. The nonlinear dynamics were studied here in two simple contexts: with a uniform SST (section 3) and with a warm-pool SST (section 4).

With a uniform SST, the model’s nonlinear dynamics were studied in the simplest context. For an initial wavenumber-2 MJO, a coherent MJO signal emerged with the fundamental features 1–3 of the MJO skeleton, with both enhanced and suppressed phases of convective activity, and with significant fluctuations of 1–3 K day^{−1} in the maximum convective activity. Moreover, this nonlinear MJO structure is asymmetric: the enhanced convective region is narrower and has a larger amplitude than the suppressed convection region. Two other cases displayed further nonlinear dynamics of the MJO modes by including multiple MJO wavenumbers initially. These cases showed nonlinear variations in the number, strength, and/or locations of MJO events, such as a strong MJO event followed by a weaker MJO event, similar to TOGA COARE.

With a warm-pool SST, MJO events often began as standing oscillations and then propagated slowly eastward across the warm pool. While displaying the fundamental features of the MJO skeleton, these MJO events had significant variations in their lifetimes and regional extents, and they displayed intense, irregular fluctuations in their amplitudes. In addition, the MJO events interacted with high-frequency “dry” Kelvin and equatorial Rossby waves, often with these waves appearing to “trigger” or “terminate” an MJO event, and/or with these dry waves appearing to be “ejected” into the cold pool. Furthermore, some details of the phase relationships in the MJO skeleton are rectified to a degree. This was illustrated by instances of collocated anomalies of convective activity and lower-tropospheric moisture and by collocated anomalies of convective activity and westerlies, the latter in resemblance of a westerly wind burst in the final stages of an MJO event. In other cases with a warm-pool SST, an initial dry disturbance excited the low-frequency moist waves, both eastward and westward propagating. The eastward-propagating mode dominated most of the warm pool, whereas the westward-propagating mode dominated the cold pool and far western parts of the warm pool. As corroboration of the previous linear theory results, the nonlinear moist Rossby mode did not have enhanced amplitude over the warm pool, suggesting that it is not as strongly coupled to moist convective processes as the MJO mode.

While this nonlinear oscillator model is able to capture all of the features of the MJO skeleton summarized above, several finer details of the MJO’s “muscle” are not included in this model. These details include, for instance, a refined vertical structure (Lin and Johnson 1996; Myers and Waliser 2003; Kikuchi and Takayabu 2004; Kiladis et al. 2005; Tian et al. 2006); stronger circulation anomalies, such as a westerly wind burst; upscale momentum transport from mesoscale convective systems and synoptic-scale convectively coupled equatorial waves (Moncrieff and Klinker 1997; Houze et al. 2000; Tung and Yanai 2002a,b; Majda and Biello 2004; Biello and Majda 2005; Majda and Stechmann 2009a); and the effect of land–sea contrasts and surface fluxes (Sobel et al. 2008, 2010). Moreover, the nonlinear oscillator model presented here is a model for only the intraseasonal/planetary-scale features of the MJO. A more complete model should also resolve the detailed subplanetary-scale features within the MJO’s envelope of convective activity, including synoptic-scale convectively coupled equatorial waves and/or mesoscale convective systems (Nakazawa 1988; Hendon and Liebmann 1994; Dunkerton and Crum 1995; Yanai et al. 2000; Houze et al. 2000; Masunaga et al. 2006; Kiladis et al. 2009), depending on the model resolution.

The authors thank two anonymous reviewers for comments that improved the clarity and presentation of the paper. The research of AJM is partially supported by Grants NSF DMS-0456713, ONR N00014-08-1-0284, and ONR N00014-11-1-0306. SNS was supported by a NOAA Climate and Global Change Postdoctoral Fellowship, a NSF Mathematical Sciences Postdoctoral Research Fellowship, and a start-up grant from the University of Wisconsin—Madison.

# APPENDIX

## Alternative Model with Weak-Temperature-Gradient Approximation

*q*equation in (3) to yield equations for

*q*and

*a*′ alone:where the

*a*equation has been linearized. This is the ordinary differential equation of a simple harmonic oscillator with frequency given by (A1). While the weak-temperature-gradient approximation gives this result in a simple fashion, it also has important limitations. For instance, it is not clear that this weak-temperature-gradient approximation is valid on intraseasonal/planetary scales (Majda and Klein 2003); a valid weak-temperature-gradient approximation is the Seasonal Planetary Equatorial Weak-Temperature-Gradient (SPEWTG) model of Majda and Klein (2003), but it actually appears on somewhat smaller-than-planetary spatial scales and on intraseasonal-to-seasonal time scales. In addition, and more importantly, the dynamics loses its east–west asymmetry; that is, since

*ω*

^{2}is given by the constant in (A1), both the eastward- and westward-propagating low-frequency modes have the same oscillation frequencies, in contrast to the results in Fig. 2.

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