Open access peer-reviewed chapter

# Interaction of Tropical Cyclones with a Dipole Vortex

Written By

Ismael Perez‐Garcia, Alejandro Aguilar‐Sierra and Jaime Hernández

Submitted: 15 March 2016 Reviewed: 26 September 2016 Published: 01 March 2017

DOI: 10.5772/65953

From the Edited Volume

## Vortex Structures in Fluid Dynamic Problems

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## Abstract

The purpose of this chapter is to discuss certain disturbances around the pole of a Venus–type planet that result as a response to barotropic instability processes in a zonal flow. We discuss a linear instability of normal modes in a zonal flow through the barotropic vorticity equations (BVEs). By using a simple idealization of a zonal flow, the instability is employed on measurements of the upper atmosphere of Venus. In 1998, the tropical cyclone Mitch gave way to the observational study of a dipole vortex. This dipole vortex might have helped to intensify the cyclone and moved it towards the SW. In order to examine this process of interaction, the nonlinear BVE was integrated in time applied to the 800–200 hPa average layer in the previous moment when it moved towards the SW. The 2‐day integrations carried out with the model showed that the geometric structure of the solution can be calculated to a good approximation. The solution HLC moves very fast westwards as observed. On October 27, the HLA headed north‐eastward and then became quasi‐stationary. It was also observed that HLA and HLC as a coupled system rotates in the clockwise direction.

### Keywords

• polar vortices Venus
• barotropic vorticity equation
• normal mode instability
• tropical cyclone
• American monsoon system.

## 1. Introduction

The air at the equatorial regions rises when heated by the sun and as it does, it cools down and sinks. Rising air creates low pressure, sinking air creates high pressure. High altitude winds move towards the poles and surface winds move towards the equator, creating a simple convective motion known as the Hadley cells. These Hadley cells are the atmospheric circulation system driven by solar heated ground. On Earth, the Coriolis effect breaks each circulation cell into several separate cells, which are easily visible from space. Global circulation or local weather systems moves from West to East at mid–latitudes in the Northern Hemisphere (NH). Two main factors that cause these patterns are atmospheric heating and planetary rotation.

Vortices are structures observed in planets with atmospheres. Earth, Mars, Venus, Jupiter and Saturn. On Earth, these atmospheric vortices are called cyclones and anticyclones. A cyclone or “Low” is a storm or a system of winds that rotates around a centre of low atmospheric pressure. An anticyclone or “High” is a system of winds that rotates around a centre of high atmospheric pressure.

Winds in a cyclone blow counterclockwise in the NH while they move clockwise in the Southern Hemisphere (SH). Winds in an anticyclone blow in the opposite direction. Cyclones that form over tropical regions are called tropical cyclones. The semi‐permanent and transient cyclones or anticyclones are associated with weather systems. Polar vortex, Bermuda High, the Siberian High and the Aleutian Low are examples of semi‐permanent systems. The subtropical high pressure belts that exist in the atmosphere overlaps with the descending legs of the Hadley cells. These semi‐permanent subtropical centres of high pressure develop as direct responses to solar heating produced by the differential heating of continents and oceans. The role of the cyclones and anticyclones in the general circulation of the atmosphere is to exchange heat and moisture between the equator and the poles.

The polar vortex, also called “Circumpolar vortex”, is an upper level low‐pressure zone, with a prevailing wind pattern that circulates in the Arctic, flowing from west to east lying near the Earth's pole, that is usually kept in place by the jet stream that divides cold air from warm air. The jet stream is a relatively narrow band of strong winds in the upper levels of the atmosphere that blow from West to East; however, it often shifts to the North or South. The strongest occurrence of jet stream takes place during both the Northern and Southern Hemisphere winters. The 50°60°N/S region is where the polar jet is located with the subtropical jet near 30°N. The interface between the cold dry air mass from the pole and the warm moist air mass from the south, defines the location of the polar front, extending from the surface up to the troposphere. An upper‐level front on Earth is usually associated with the mid‐latitude jet [1], while the cold collar on Venus is a ring of cooler air that surrounds the polar vortex and which denotes a darker area between 60°and80° [2].

The Earth and Venus are about the same size. Venus has a radius of av=6051.8 km and the Earth has a mean radius a=6371 km. Venus moves around the Sun, completing one orbit in every 224 earth days. Most of the planets and the sun in our solar system rotate in the counter‐clockwise direction when viewed from above their North Poles. Venus, however, rotates in the opposite direction. Venus spins extremely slowly, completing one rotation every 243 earth days, so on Venus the Coriolis effect is very weak. It is also weak in Earth’s tropics. A day in Venus is longer than its year. Venus's retrograde turn means that the planet's North Pole actually lies below the ecliptic plane.

The atmosphere on Venus is extremely dense, the temperature increases downwards from 100 to 40 km except in an inversion layer about 6070 km. The range of 1360 mbar have altitudes of 55–85 km, with surface pressures of 90 mbar and clouds beginning at 43 km [3]. In 1974, a hemispheric vortex centred at the South Pole of Venus was observed at the time of Mariner 10. In 1979, images of Venus from Pioneer showed a similar vortex at North Pole. The winds were stronger at the equator, and slowed down towards the poles, creating a visible “V” shape on images of the cloud layers. In fact, the Venus clouds upper‐deck rotates around the planet in just 4–5 days, which is in a much faster pace than in the underlying surface [4]. This is called super‐rotation, because it is in the same direction as the rotation of the planet, but much stronger. The super‐rotation is not that of an actual rigid body. Two essential questions remain to be answered: what are these eddies at the polar region? Where do they come from? They come from the processes of barotropic instability [5]. In Section 2, the fact that certain disturbances around the Venus pole arise as a response to barotropic instability processes of a zonal flow is demonstrated.

On Earth, tropical cyclones originate over tropical or subtropical regions in the Indian Ocean, western North Pacific and South Pacific Ocean, forming between 5°and30° N and typically move westwards, north and north‐westwards. When tropical cyclones reach subtropical latitudes, they often move north‐eastwards. Also, the coasts of Mexico and Central America are influenced by the presence of the northern Atlantic and north‐eastern Pacific tropical cyclones. A question remains to be answered on the movement of tropical cyclones: what pushes them south‐westward. In particularly, tropical cyclone Mitch moved south‐westward by October 26–30, [6]. The overall motion of Mitch was slow, less than 5 mph, this resulted in a tremendous amount of rainfall, primarily over Central America, which killed thousands of people. Section 3 of this present chapter, provides an observational study of a dipole vortex associated with the tropical cyclone Mitch, and the barotropic vorticity equations (BVEs) used to study the movement toward Southwest. The dipole vortex is an interesting feature that occurs during the intersection of the local summer months (September–November), formed in coupled monsoon systems: the late North American monsoon system (NAMS) and early South American monsoon system (SAMS).

## 2. Polar vortices in planetary atmosphere

A polar vortex, also known as the “Circumpolar Whirl”, is a large‐scale circulation in the middle and upper troposphere, generally centred in the Polar Regions. These polar vortices form when heated air from equatorial latitudes rises, and then spirals towards the poles. In fact, the upper deck of clouds on Venus rotates around the planet much faster than the underlying surface. This is also called super‐rotation, because the rotation is in the same direction as the rotation of the planet, but faster [4].

At the cloud top altitude of 6772 km, the main properties of the mean zonal velocity profile are well known. Hueso and Sanchez‐Lavega [3] presented an update on the average zonal and meridional mean profile wind of the upper cloud at 6673 km for Venus SH from 90° to near 5° as observed with VIRTIS‐M UV day‐side data. Comparing with previous results by Sanchez‐Lavega [7] and Moissl [8], they present the same general behaviour at all altitudes. Moissl [8] showed that a profile zonal wind from 85° to 20° with a zonal wind speed of 85°90 m/s almost constant with latitude is observed at low latitudes. The latitude zonal wind profile shows a gradually increase reaching 100 m/s near 45°S, indicating the presence of a weak midlatitude jet. South of this latitude the wind speed decreases to zero towards the poles.

We assume that there is a similar circulation in the Northern Hemisphere in Venus, as observed in the “V” shaped clouds that move westwards. Therefore, we may be reconstructing a simple idealization of a symmetric zonal flow around Venus’ equator based on the measurements taken from the upper atmosphere of Venus broadly consistent with the work of Refs. [3, 7, 8, 9]. This latitude profiles of symmetric zonal wind at the upper cloud layer at 6673 km is shown in Figure 1.

In latitudes between 50°and  50°, strong winds of up to 100m/s with ±10m/s oscillations were observed. In latitudes between 4° and 4° strong winds of up to 108m/s were observed, indicating the presence of a weak jet near the equator. Zonal winds closer to the poles gradually slowdown at latitude of about 48° on Venus. In both the Northern and Southern Hemispheres a small jet stream was found along with a meridional shear of uy=0.027 ms1 km1 [3].

Venus’ atmosphere can be divided into two broad layers. The first layer rotates in 4 Earth days and the second one is underneath. Let the height of Venusian atmosphere be Hv, we may consider that the Venusian atmosphere resides between two concentric spheres with different radii av and avt=av+Hv. Assuming that the mean level of this spherical shell rotated around the planet in just 4 Earth days or at an angular velocity Ωva=2.893×106 s1, it would be much faster than the underlying surface or Venus angular velocity Ων=3×107s1.

Widely used to understand many features of the large scale dynamics of the barotropic Earth atmosphere, we might consider the vertical component of the barotropic vorticity equation (BVE) for an ideal fluid non‐divergent on a unit sphere S, which can be written in the non‐dimensional form as follows [10]:

ΔΨt+J(Ψ,ΔΨ+2μ)=0E1

where Ψ(λ,μ) denotes the stream function. The spherical coordinates are longitude λ,latitudeϕ or μ=sinϕ,πλπ,π2ϕπ2. Δ is the Laplace operator on a sphere and J(Ψ,η) is the Jacobian operator. The equation is non‐dimensionalized with the Earth radius a as the length scale and the inverse of the Earth angular velocity 7.292×105 s1 as the timescale. The relative vorticity is ξ=ΔΨ and the absolute vorticity is η=ξ+2μ. On Venus, the Coriolis parameter would be neglected, since it is two orders of magnitude lower than the Earth’s one. The relative vorticity expressed in terms of wind vector (u,v):

ξ(λ,μ)=11μ2νλ1μ2uμ+μu1μ2E2

Where

u=1μ2Ψμ,ν=11μ2ΨλE3

are the velocity components that relates to the stream function.

Eq. (1) captures many features of the large scale dynamics of the barotropic Earth’s atmosphere, providing better understanding of the low–frequency variability, teleconnection patterns and the synoptic blocking events [1115]. A mechanism that generates low‐frequency variability is the instability of non‐zonal basic flow as proposed by Simmons et al. [11]. The four classes of BVE (for ideal flow) solutions known by now are the simple zonal flows Ψ˜(μ) and more complicated flows called Rossby–Haurwitz (RH) waves, Wu–Verkley waves [16] and modons [1721].

The temperature and pressure on Earth are similar to those above 50 km on Venusian atmosphere. This implies that Earth's BVE can be applied to Venus middle atmosphere [2, 5]. The instability caused by the existence of a sufficiently large horizontal shear in the wind field of a basic flow is known as barotropic instability [22]. In continuation with the study of that polar dipole vortex might result from the barotropic and baroclinic instabilities of the Venusian atmosphere [5, 2325]. We were interested in exploring the instability of a zonal flow in super‐rotation and the instability of zonal basic flow as shown in Figure 1.

In order to examine the resulting perturbation in the linear barotropic model, Skiba and Perez–Garcia [26] developed a numerical spectral method for normal mode stability study of ideal flows on a rotating sphere, which was tested on zonal flows [27].

The linearized equation for ξ' is:

ξ't+J(Ψ˜,ξ'+2μ)+J(Δ1ξ',ξ˜+2μ)=0,E4

Where ξ'=Δψ' is relative vorticity of the perturbation, the wide tilde mark represents basic flow, and primes refer to infinitesimal perturbation. In the form of a normal mode

ψ'(λ,μ,t)=Ψ^(λ,μ)eωt,ξ'(λ,μ,t)=ΔΨ^(λ,μ)eωt=G(λ,μ)eωt,E5

LG=ωGE6

For the linearized operator LG=J(G˜1G)J(Ψ˜,G), ω=ωr+iωi, is the eigenvalue, G the eigenfunction and Ψ^(λ,μ)=Ψ^r(λ,μ)+iΨ^i(λ,μ)=|Ψ^(λ,μ)|eiθ is the amplitude. Here θ(λ,μ)=argθ(λ,μ)=arctan{Ψ^r(λ,μ)Ψ^i(λ,μ)} is the initial phase of the mode. In the normal mode (linear) stability analysis, the basic state must be regarded as a steady state. A mode ψ' is unstable if ωr>0, decaying if ωr<0, neutral if ωr=0, and stationary if ωi=0.

A zonal basic flow with horizontal shear can be constructed analytically by Ψ˜(μ)=wPn(μ) in which Pn(μ) is a Legendre Polynomial (LP), with μ=sinϕ, and w, an arbitrary constant. The simplest super‐rotation zonal flow is analytically constructed so that the equatorial easterly jet streams (the mean zonal wind in the equatorial latitude is 105m/s decreasing to zero at the pole) are preserved with a weak easterly wind around poles: Ψ˜(μ)=wP1(μ)=wμ(w=0.226is the rotation velocity). We used the Rayleigh‐Kuo necessary condition for the instability [28, 29]: Let Ψ˜(μ) be a zonal flow on the sphere, then a normal mode may be unstable only if the derivative η˜μ of the absolute vorticity η˜=Ψ˜(μ)+2μ changes its sign at least in one point of the interval (1,+1). Since in the mean level of Venus’ atmosphere the absolute vorticity η˜=Ψ˜(μ)+2rμ, where r=3.96×102, then in our case, η˜μ=2(w+r) is a constant and hence there is no unstable normal mode, this is neutral. However for the zonal flow Ψ˜(μ)=wPn(μ),η˜μ=2rwχnPnμ where χn=n(n+1), then there is a critical amplitude w for developing the instability, due to the sphere rotation [26, 27].

Rossby‐Haurwitz wave has proved to be very useful in interpreting the large‐scale wave structures in the Earth atmospheric circulation of middle latitudes. Not only should the zonal wind profile be consistent with Venusian climatology (Figure 1), but attention must also be given to the absolute vorticity of the zonal flow in the equatorial region. The effect of the mean flow, given by a linear combination Legendre polynomials and a Rossby‐Haurwitz wave, was provied by Refs. [15, 27]. The zonal basic flow, demonstrated in Figure 2, can be approximated by the following,

Ψ˜(μ)=j=05w2j+1P2j+10(μ)+j=12w2jP2j0(μ),E7

where Pnm(μ) is the associated Legendre function of degree n and zonal wave number m, and w' are constants and w5 is very small. Then,

η˜μ=2rj=05χ2j+1w2j+1P2j+10μj=12χ2jw2jP2j0μE8

changes its sign at least in one point of the interval (1,+1), and thus Eq. (7) may have unstable normal modes.

Observational evidence indicates that the zonal flow pattern on the Earth can be approximately represented by a linear combination of seven Legendre polynomials of odd parity [15, 30]. The zonal flow has the maximum westerly of 33 m/s at 35° North and South, and an easterly wind of 5 m/s at the equator. This zonal wind field resembles the upper troposphere during the northern winter. The stability analysis showed that unstable perturbations are observed in the neighbourhood of subtropical jets, and the dominant zonal wave number of the modes are m=7 and m=5 (see Figure 3 of [15]).

However, Skiba [31] showed that for a zonal flow PL and a RH wave, the amplitude Ψ^, of each unstable or decaying mode must satisfy the condition,

χΨ^=E(Ψ^)k(Ψ^)E9

where χΨ^ is the square of Fjörtoft's [32] average spectral number of the mode amplitude Ψ^, and K(Ψ^)=12Ψ^2=12n=1χnm=nn|Ψ^nm|2 and E(Ψ^)=12ΔΨ^2=12n=1χn2m=nn|Ψ^nm|2 are the total kinetic energy, and entrophy of Ψ^, and Ψ^nm is the Fourier coefficient.

In this part of our chapter we shall study the normal mode numerical stability, in the case of zonal flow in Figure 1, then Eq. (6) is solved by representing all variables as series of spherical harmonics, by employing triangular truncation T21 and by taking the Coriolis parameter as 2rμ. The main parameters of the first four most unstable modes, ω=ωr+iωi, spectral number χΨ^ of the mode amplitude, e‐folding time τe=12π|ωr| and period T=1|ωi| of the mode are given in Table 1.

ModesωrωiχΨ^τeT
186.03215.5386.261.84×103,4.63×103,
264.28309.5289.392.47×103,3.23×103,
357.16236.4576.942.78×103,4.22×103,
447.6366.0156.553.34×103,1.51×102,

### Table 1.

The most unstable mode of the Venus’ polar zonal flow described by Figure 2.

As shown in Figure 2, for the first two most unstable modes, disturbances are located at the northern side of the largest jet stream of the North Hemisphere and for the third most unstable mode the disturbances are generated at the southern side of the largest jet stream in the South Hemisphere. From Ref. [26] we get the equation that describes the evolution of the total kinetic energy K(ψ') of an infinitesimal perturbation ψ' to a zonal flow Ψ˜(μ) on sphere S,

dK(ψ')dt=1u2(u'v')u˜μdsμ1μ2(u'v')u˜dsE10

The sign of dK(ψ')dt depends on the signs of the products (u'v')u˜ and (u'v')u¯μ in various regions of the sphere. In regions of generation of the energy of perturbations, the inclination of main axes of localized perturbations in the stream function field must be opposite to the inclination of zonal velocity profile, that is, in the regions where product (u'v')u¯μ is positive [11]. Whereas the first integral dominates principally at the sides of the jets located in the tropics and mid‐latitudes, the second integral can be significant in the central parts of strong jets, especially when such jets are located in the polar regions, where μ1μ2 is large [26, 27]).

Figure 2(d) shows the four modes most unstable with the V shapes, along the equatorial region. Data from the Vertis on Venus Express [33], also near the equator, show that similar “V” structure of cloud layers were observed, as shown in this chapter, which could be associated with the barotropic instability processes. Further experiments were performed with different values for r=ΩvΩ=0 (the Coriolis parameter neglected). The results proved to be similar to those presented in Table 1. So the generated unstable disturbances are due to intense zonal wind shear.

Unstable perturbation or vortices behaviour develops in the polar regions of Venus as a response to processes of barotropic instability of a zonal flow. These results are consistent with earlier studies of barotropic instability on Venus given in Refs. [24, 34, 35] and others, who were seeking a possible origin for the Venus polar dipole features observed by Pioneer Venus.

New data of zonal wind of the middle atmosphere to cover a wide range of latitudes in the NH will help to know about the unstable perturbation that develops in the polar regions of Venus NH as a response to processes of barotropic instability. It has been shown that the Venus polar dipole is a permanent feature in the Venusian atmosphere and that it is confined to latitudes higher than 75° S [25, 33].

Simmons et al. [11] showed that barotropic instability can be responsible for a low‐frequency variability of Earth's atmosphere, and Perez‐Garcia [15] demonstrated that unstable perturbations are observed in the neighbourhood of subtropical jets on the Earth. Then an analytic dipole vortex may be constructed on the Venus Polar Regions. This would be called a Verkley's polar modon [17] with different dynamical configurations. Venusian atmosphere has given us not just the opportunity to learn from this initial work, but also to continue research on this topic. Our next challenge is to analyse the barotropic instability of the Zonal Flow seen in Figure 1, coupled with Verkley’s polar modon.

## 3. Global monsoon system, tropical dipole vortices and tropical cyclones

NCAR‐ds627.0 and NCEP/NCAR Reanalysis data were used. In particular, we used the relative humidity, the zonal (u) and meridional (v) components of the wind field at different pressure levels. These wind components are further used in the calculation of their corresponding velocity potential and stream function.

Figure 3 shows the mean of 200250 mbar stream function monthly and tropical cyclone tracks for April. A noticeable feature in Figure 3(a) is the basic patterns of the circulation associated with monsoon land heating at the equator in the African region monsoon, 10°40°E, Asian‐Australian monsoon, 60°180°E and South‐American monsoon, 80°40°W. The Australian summer monsoon influences the climate of the Australian tropics during the period of December–March [37]. The onset of the Australian summer monsoon occurs in late December and typically retreats in April [38].

The early arrival of the Indian summer monsoon and North American early summer monsoon are shown in Figure 3(b). The wet season of the Asian monsoon system begins in May and ends in October and the dry phase occurs in the other half of the year [39]. The set of these local monsoon systems is called the global monsoon system [40]. Liu and Zorita [41] defined the local summer as May through September (MJJAS) in NH and November through March (NDJFM) for SH.

The American monsoon is determined by the dynamic processes of the interaction between the American continent, the eastern Pacific, the Atlantic Ocean and the overlying atmosphere [42]. The intense heat from the land creates rising of air and a surface low pressure, with low‐level air flowing towards the convective regions and divergence in the upper troposphere, then the tropical cyclone moves towards the convective regions of the heated continents (Figures 3(a) and 4(b)).

An important feature of the upper troposphere of a monsoon system is the high‐level anticyclone (HLA) located above and to the north of the monsoon trough. The clockwise flow around this anticyclone contains an easterly jet stream in its southern flank called tropical easterly jet [43] and in the lower troposphere, for example, in North America late summer contains a maritime‐continental thermal low (Figure 5).

In the Indian Ocean, the tropical cyclones mainly occur during pre‐monsoon and post‐monsoon seasons. In western North Pacific, TC most generally begins from June and ends in November [44]. Gray [45] estimates that the majority of TCs originate in or are just polewards of the Intertropical Convergence Zone [ITCZ] or monsoon trough. The upper tropospheric flow patterns over the region of storm formation control their formation and movement. Some storms recurve under the influence of a high‐level anticyclone or an approaching westerly troughs of middle latitudes that extends into the upper levels of lower latitudes where east winds occur in the surface layers.

In the Atlantic Ocean, the tropical cyclones mainly occur during May–October. In the lower troposphere, westward traveling tropical wave disturbances move in the trade wind flow across the Atlantic Ocean. They begin appearing as early as April/May and continue until October/November. Burpee [46] documented a mechanism for the origins of these waves, the instability of the African easterly jet.

An interesting feature occurs during months of May, September‐November in the American monsoon system, in which its upper levels are formed with an anticyclone HLA on the northern side and an anticyclone HLC (high‐level cyclone at NH) on its southern side. As a result, in certain periods, for example between September and November, the HLC and HLA remain coupled and then form a bipolar vortex or coupled monsoon system North American monsoon system (NAMS) late, and South American monsoon system (SAMS) early [6]. This bipolar vortex has a similar configuration to the Gill‐Matsuno wave [47].

The genesis of Mitch was given by Refs. [6, 4850]. In this chapter, we are interested in studying its trajectory. Why did it changed its direction south‐westward during the period of October 26–28, 1998? And how the interaction with HLA and HLC may have contributed to change its path south‐westward? Due to the variation of the Coriolis parameter, a cyclone embedded in a resting atmosphere moves north‐westwards [51].

In Figure 6(a) and (c) we get a general idea that the trajectory HLA and HLC took. By October 26–27, 00Z, HLA acquired a movement almost axi–symmetric with a north‐eastern flow on its southeast side. HLC was moving west‐north‐westward very quickly, while HLA headed north‐eastward, merging together as a coupled system (Bipolar Vortex), apparently starting an anticyclonic rotation (Figure 6(ac)). Because Mitch was much closer to HLA, it was guided by the HLA circulation.

On October 26th HLA was situated on the Mexican plateau along with three other anticyclone disturbances, while HLC also had three more perturbations involved with it. The tracks of HLA and HLC and their multiple disturbances by October 27 are shown in Figure 6(b), merging together, demonstrating their clockwise rotation.

During October 27–28, HLA changed direction, returning south‐westward; however, HLC dispersed in a westward direction. In order to examine these interaction processes, the numerical spectral of nonlinear barotropic model (1), in truncation T31, was integrated in the time, with the initial stream‐function corresponding to October 26th‐00Z, 800–200 mbar mean layer (see Figures 6(a) and 7(a)).

The 2‐day integrations carried out with the model show that the geometric structure (comparing Figures 6 and 7) of the solution can be calculated to a good approximation. On October 27th, the solution HLC moved westward very fast, while HLA headed north‐eastward and then became quasi‐stationary. Also, HLA and HLC as a coupled system rotated in a clockwise direction as given in Figure 6(c).

The formation, development and evolution of the tropical cyclone Mitch was not a process by which isolated vortices were solely involved, but rather a result of a very complicated and precise conditions, which interacted among themselves and by nearby flows. In the case described here, these nearby flows were associated with the bipolar vortex formed by late NAMS and early SAMS.

## Acknowledgments

The authors are grateful to A. Salas, E. Azpra, F. Villacaña, O. Delgado, R. Patiño and L. Meza for the map analysis. We thank Nat Aguilar and an anonymous reviewer for their useful comments that helped to improve the manuscript. The data was provided by NCAR's Data Support Section (DSS). The National Science Foundation is NCAR's sponsor.

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Written By

Ismael Perez‐Garcia, Alejandro Aguilar‐Sierra and Jaime Hernández

Submitted: 15 March 2016 Reviewed: 26 September 2016 Published: 01 March 2017