# A Novel Technique for Predicting the Thermal Behavior of Stratospheric Balloon

Authors: Yunpeng Ma; Jun Huang; Mingxu Yi
Journal: International Journal of Aerospace Engineering
 (2018)

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## Abstract

This paper is devoted to introduce a novel method of the operational matrix of integration for Legendre wavelets in order to predict the thermal behavior of stratospheric balloons on float at high altitude in the stratosphere. Radiative and convective heat transfer models are also developed to calculate absorption and emission heat of the balloon film and lifting gas within the balloon. Thermal equilibrium equations (TEE) for the balloon system at daytime and nighttime are shown to predict the thermal behavior of stratospheric balloons. The properties of Legendre wavelets are used to reduce the TEE to a nonlinear system of algebraic equations which is solved by using a suitable numerical method. The approximations of the thermal behavior of the balloon film and lifting gas within the balloon are derived. The diurnal variations of the film and lifting gas temperature at float conditions are investigated, and the efficiency of the proposed method is also confirmed.


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## Body

## 1. Introduction

Stratospheric balloons or airships have been paid attention since they can provide persistent observation platforms by keeping on station at an altitude about 20~30 km for a long time. They have some potential advantages, such as station keeping, long endurance, low cost, broadcasting, and telecommunication relay [1–3]. When the balloons stay at an altitude about 20~30 km, they should be filled with a huge gas volume of several hundred thousand cubic meters. Even a small temperature variation between the inner gas and the outer environment can lead to a huge buoyancy difference. So the thermal behavior of the stratospheric balloon should have attracted some interest from all over the world [4, 5].It is important to predict the thermal behavior of the stratospheric balloon before it launches. Understanding the temperature variation of the stratospheric balloon will be helpful for balloon design and flight prediction. During the research of the thermal behavior of the stratospheric balloon, the average film and lifting gas temperature are the main focus. Carlson et al. [6] studied the trajectory and thermal behavior of the high-altitude balloons. Stefan [5] used a two-node model to solve the day-night airship temperature numerically. Farley [7] established a code to calculate the ascent and float thermal behavior of the stratospheric balloon. Dai et al. [8] developed a simulation program to investigate the thermal performance of a super pressure balloon by using the thermal models and dynamic models. Yao et al. [9] proposed a multinode heat transient model for stratospheric airships to predict the thermal behaviors of the ascent and descent processes. In these articles, the thermal models are established for different conditions. The thermal performance of the film and lifting gas can be obtained by solving TEE. The main method to solve these equations is discrete collocation method. The computation efficiency is low when the number of surface elements of film are very large.In this paper, we adopt the thermal models given by Xia et al. [10] and present a novel technique to solve the TEE. The thermal performance of the film and lifting gas will be got by applying the method to solve the TEE. The method is based on Legendre wavelet integration operational matrix method. In the proposed method, the TEE is reduced to a system of nonlinear algebraic equations, which can be solved easily. The proposed method is of high computing efficiency and simple operation.


## 2. Thermal Model

In this section, the same thermal environment and assumptions of the stratospheric balloon shown in [11, 12] will be considered. The thermal environment (shown in Figure 1) of the high-altitude stratospheric balloon includes infrared radiation, solar radiation, and convection. The balloon film is so thin that the conductive resistance can be neglected.Figure 1
Thermal environment of a stratosphere balloon.The transient temperature distribution of the film is expressed by the following [10]:
(1)δtρc∂T∂t=hexTa−T+hinTg−T+∑i=13qi−εexσT4+αinG−εinσT4,where δt,ρ,andc are the film thickness, density, and specific heat, respectively. hex and hin are the convective heat transfer coefficients for the external and internal surfaces of the film. T,Ta,andTg are the film temperature, atmosphere temperature, and lifting gas temperature, respectively. qii=1,2,and3 are the absorbed direct solar radiation, the absorbed diffuse solar radiation, and the absorbed reflected solar radiation. εex and εin are the external and internal emissivities of the film. αin denotes the internal absorptivity. G is the total irradiation falling on the film. σ is the Stefan Boltzmann constant.The total irradiationG at the internal film segment r→i can be obtained by the following:
(2)Gr→i=∑k=1MsJkFi,k,where Fi,k is the angle factor from element i to element k. Ms is the total number of surface elements of the balloon. Jk is the infrared radiation away from the internal surface, and it can be calculated as follows:
(3)Jk=εinσT4r→k+1−αinGr→k.Then the average temperature of the lifting gas is written in the following equation [8]:
(4)cgmg∂Tg∂t=∫ShinT−TgdS,where cg is the specific heat. mg is mass of the lifting gas.


### 2.1. Atmosphere Model

The relation between the atmosphere temperature, pressure, and the altitude are given by the following [13]:
(5)Ta=288.15−6.5H,0≤H≤11000m,216.65,11000m≤H≤20000m,216.15+H−20,20000m≤H≤32000m,Pa=1013251−H443305.26,0≤H≤11000m,22606e11000−H/6340,11000m≤H≤20000m,2447141.89+0.003H216.65−11.388,20000m≤H≤32000m,where H is the altitude of the balloon.


### 2.2. Solar Position and Solar Radiation Models

Before we introduce the solar radiation models, the computational method of solar position should be given as follows.Suppose thatη denotes the solar altitude angle and ψ denotes the solar azimuth angle, then we have the solar direction vector
(6)mx,my,mz=cosηcosψ,cosηsinψ,sinη.The solar altitude angleη and the solar azimuth angle ψ can be expressed by the following [14]:
(7)α=arcsinsinδsinϕ+cosδcosϕcosω,ψ=arccossinϕsinη−sinδcosηcosϕ,where ϕ is the local latitude, δ is the declination of the sun, and ω is the hour angle of the sun. They are defined as
(8)δ=180π0.006918−0.399912cosΓ+0.070257sinΓ−0.006758cos2Γ+0.000907sin2Γ−0.002697cos3Γ+0.00148sin3Γ,ω=36024+Et12+Et2,where Γ is solar day angle and Et is the value of time correction. The calculate method will be
(9)Γ=2πdn−1365,Et=229.18600.000075+0.001868cosΓ−0.032077sinΓ−0.014615cos2Γ−0.04089sin2Γ,where dn is the day of the year.The absorbed direct solar radiation heat flux is shown as [15]
(10)q1=δsαsτsEscosβ,where δs is the index which considers the self-shadowing and δs=1 is the direct solar radiation; otherwise, δs=0. αs is the solar absorptivity of the external surface. τs is the atmosphere transmissivity. Es=1353W/m2 is the solar constant. β is the included angle between the solar radiation and surface external normal.The absorbed diffuse and reflected solar radiation heat flux is written as [16]
(11)q2=αsEsγ+ρeτsFe,where γ is the empirical diffuse coefficient. ρe is the Earth’s reflectivity. Fe is the angle factor between the film and the Earth.The infrared radiation heat flux from the Earth and atmosphere can be given by [16]
(12)q3=αexτatmqeFe,where αex is the absorptivity of the external surface in the infrared spectrum. τatm is the transmissivity of the atmosphere in the infrared spectrum. qe is the Earth’s atmosphere infrared flux.


### 2.3. Convective Heat Transfer Coefficient Models

Convective heat transfer happens to both inner and external surfaces of the balloon hull. For the inner surface, the heat convection is usually considered as a natural convection. For the external surface, the heat convection is either a forced one or natural one. It depends on the relative speed of the balloon and the atmosphere characteristic. According to the theory of Leland and Walter [17], the convective heat transfer coefficients for both inner and external surfaces are calculated by
(13)h=NuλL,where Nu is the Nusselt number, λ is the thermal conductivity of the gas, and L is the length of the balloon.For the inner surface, the Nusselt numberNu is
(14)Nu=2.52+0.6Ra1/4,0≤Ra≤1.5×108,Nu=0.325Ra1/3,Ra>1.5×108.For the external surface, natural convection case, Nusselt numberNu is
(15)Nu=2+0.6Ra1/4,0≤Ra≤109.For the external surface, forced one, Nusselt numberNu is
(16)Nu=0.37Re0.6,10<Re<105,Nu=0.74Re0.6,Re>105,where Ra is Rayleigh number and Re is Reynolds number. They can be obtained by
(17)Ra=Gr⋅Pr,Gr=gnξΔTL3υ2,Re=VLυ,where Gr is the Grashof number, Pr is Prandtl number, gn is the gravitational acceleration, ξ and υ are the coefficient of thermal expansion and the kinematic viscosity, respectively, ΔT is the temperature difference between the surface and the gas, and V is the airspeed of the balloon. The kinematic viscosity υ can be got as follows:
(18)υ=μρ,where μ is the dynamic viscosity. The computational method of these parameters (λ,μ,andPr) for helium and air will be found in [18].


## 2.1. Atmosphere Model

The relation between the atmosphere temperature, pressure, and the altitude are given by the following [13]:
(5)Ta=288.15−6.5H,0≤H≤11000m,216.65,11000m≤H≤20000m,216.15+H−20,20000m≤H≤32000m,Pa=1013251−H443305.26,0≤H≤11000m,22606e11000−H/6340,11000m≤H≤20000m,2447141.89+0.003H216.65−11.388,20000m≤H≤32000m,where H is the altitude of the balloon.


## 2.2. Solar Position and Solar Radiation Models

Before we introduce the solar radiation models, the computational method of solar position should be given as follows.Suppose thatη denotes the solar altitude angle and ψ denotes the solar azimuth angle, then we have the solar direction vector
(6)mx,my,mz=cosηcosψ,cosηsinψ,sinη.The solar altitude angleη and the solar azimuth angle ψ can be expressed by the following [14]:
(7)α=arcsinsinδsinϕ+cosδcosϕcosω,ψ=arccossinϕsinη−sinδcosηcosϕ,where ϕ is the local latitude, δ is the declination of the sun, and ω is the hour angle of the sun. They are defined as
(8)δ=180π0.006918−0.399912cosΓ+0.070257sinΓ−0.006758cos2Γ+0.000907sin2Γ−0.002697cos3Γ+0.00148sin3Γ,ω=36024+Et12+Et2,where Γ is solar day angle and Et is the value of time correction. The calculate method will be
(9)Γ=2πdn−1365,Et=229.18600.000075+0.001868cosΓ−0.032077sinΓ−0.014615cos2Γ−0.04089sin2Γ,where dn is the day of the year.The absorbed direct solar radiation heat flux is shown as [15]
(10)q1=δsαsτsEscosβ,where δs is the index which considers the self-shadowing and δs=1 is the direct solar radiation; otherwise, δs=0. αs is the solar absorptivity of the external surface. τs is the atmosphere transmissivity. Es=1353W/m2 is the solar constant. β is the included angle between the solar radiation and surface external normal.The absorbed diffuse and reflected solar radiation heat flux is written as [16]
(11)q2=αsEsγ+ρeτsFe,where γ is the empirical diffuse coefficient. ρe is the Earth’s reflectivity. Fe is the angle factor between the film and the Earth.The infrared radiation heat flux from the Earth and atmosphere can be given by [16]
(12)q3=αexτatmqeFe,where αex is the absorptivity of the external surface in the infrared spectrum. τatm is the transmissivity of the atmosphere in the infrared spectrum. qe is the Earth’s atmosphere infrared flux.


## 2.3. Convective Heat Transfer Coefficient Models

Convective heat transfer happens to both inner and external surfaces of the balloon hull. For the inner surface, the heat convection is usually considered as a natural convection. For the external surface, the heat convection is either a forced one or natural one. It depends on the relative speed of the balloon and the atmosphere characteristic. According to the theory of Leland and Walter [17], the convective heat transfer coefficients for both inner and external surfaces are calculated by
(13)h=NuλL,where Nu is the Nusselt number, λ is the thermal conductivity of the gas, and L is the length of the balloon.For the inner surface, the Nusselt numberNu is
(14)Nu=2.52+0.6Ra1/4,0≤Ra≤1.5×108,Nu=0.325Ra1/3,Ra>1.5×108.For the external surface, natural convection case, Nusselt numberNu is
(15)Nu=2+0.6Ra1/4,0≤Ra≤109.For the external surface, forced one, Nusselt numberNu is
(16)Nu=0.37Re0.6,10<Re<105,Nu=0.74Re0.6,Re>105,where Ra is Rayleigh number and Re is Reynolds number. They can be obtained by
(17)Ra=Gr⋅Pr,Gr=gnξΔTL3υ2,Re=VLυ,where Gr is the Grashof number, Pr is Prandtl number, gn is the gravitational acceleration, ξ and υ are the coefficient of thermal expansion and the kinematic viscosity, respectively, ΔT is the temperature difference between the surface and the gas, and V is the airspeed of the balloon. The kinematic viscosity υ can be got as follows:
(18)υ=μρ,where μ is the dynamic viscosity. The computational method of these parameters (λ,μ,andPr) for helium and air will be found in [18].


## 3. Legendre Wavelets and Their Properties

The Legendre wavelet polynomials are defined on the interval0,1 as [19]
(19)ψnmt=2m+121/22k/2Pm2kt−n^,n^−12k≤t<n^+12k,0,otherwise,where k=1,2,…,n^=2n−1, n=1,2,…,2k−1, m=0,1,…,M−1 is the degree of the Legendre polynomials and M is a fixed positive integer, and Pmt are the Legendre polynomials of degree m.For any functionTt∈L20,1 may be expressed by the Legendre wavelets as follows:
(20)Tt=∑n=1∞∑m=0∞cnmψnmt,where cnm=Tt,ψnmt are the Legendre wavelet coefficients and , is the inner product of Tt and ψnmt.If (20) is truncated, then it can be rewritten as
(21)Tt≈∑n=12k−1∑m=0M−1cnmψnmt=CTΨt,where C and Ψx are m^=2k−1M column vectors, given by
(22)C=c10,c11,…,c1M−1,c20,c21,…,c2M−1,…,c2k−10,c2k−11,…,c2k−1M−1T,Ψt=ψ10,ψ11,…,ψ1M−1,ψ20,ψ21,…,ψ2M−1,…,ψ2k−10,ψ2k−11,…,ψ2k−1M−1T.We can also rewrite (21) as
(23)Tt≈∑i=1m^ciψit=CTΨt,where ci=cnm and ψi=ψnm. The index i is determined by the relation i=Mn−1+m+1. Then, we have
(24)C=c1,c2,…,cM,cM+1,…,c2M,…,cM2k−1−1+1,…,cm^T,(25)Ψt=ψ1,ψ2,…,ψM,ψM+1,…,ψ2M,…,ψM2k−1−1+1,…,ψm^T.To illustrate the effectiveness of (23), we have shown the theorem as follows.Theorem 1.
Suppose that the functionTm^t=∑i=1m^ciψit obtained by using Legendre wavelets is the approximation of Tt and Tt is with bounded second derivative, say T″t≤M~; then the series converges uniformly to the function Tt; that is,
(26)Tt=∑i=1∞ciψit.Proof. See [20].Next, we will derive the operational matrix of integration of Legendre wavelets. In order to do this, another basis set of Block pulse functions should be considered as follows [21]:
(27)bit=1,ih≤t<i+1h,i=0,1,2,…,m^−1,0,otherwise,with a positive integer value for m^ and h=1/m^.LetBt=b0t,b1t,…,bm^−1tT. Suppose that
(28)∫0tBxdx≈J⋅Bt,where J is called the Block pulse operational matrix of integration [21] and
(29)J=hΓ3122⋯2012⋯2001⋯2⋯⋯⋯⋯⋯000⋯1.The Legendre wavelets may be expanded into anm term Block pulse function as
(30)Ψt=ΦBt,where Φ=Ψt0,Ψt1,…,Ψtm^−1, ti=i/m^, and i=0,1,…,m^−1.The integration of the vector functionΨt can be expressed as
(31)∫0tΨxdx≈P⋅Ψt,where P is the operational matrix of integration. It is known (see [22]) that the matrix P can be approximated by
(32)P≈Φ⋅J⋅Φ−1.Then we have(33)∫0tTxdx≈∫0tCTΨxdx≈CTP⋅Ψt=CTP⋅ΦBt.The integrations of the functionet and sint are selected to verify the effectiveness of matrix P. The integrations of et and sint are obtained as follows ∫0texdx=et−1 and ∫0tsinxdx=1−cost. Take m^=32, the results are shown in Figure 2 and Figure 3, respectively.Figure 2
Integration ofet.Figure 3
Integration ofsint.From Figure2 and Figure 3, we can find that the matrix P is very credible to calculate the integration of any functions.


## 4. Solution Procedure for TEE (1) and (4)

In this section, the proposed method based on the Legendre wavelet expansion together with their operational matrices of integration to obtain numerical solutions of the TEE (1) and (4) is described. To obtain such numerical approximate solution, we apply the following steps:
(1)
Lett=24t~∈0,24, then dt=24dt~, t~∈0,1.(2)
Express on∂T/∂t~ and ∂Tg/∂t~ in the following form:
(34)∂T∂t~=C1TΨt~,(35)∂Tg∂t~=C2TΨt~,where C1T and C2T are unknown vector and Ψt~ is the vector which is defined in (25). By using initial conditions and integrating (34) and (35), we have
(36)Tt~=C1TPΨt~+T0,Tgt~=C2TPΨt~+Tg0.(3)
Expand the initialT0 and Tg0 by wavelets as follows:
(37)T0=X1TΨt~,Tg0=X2TΨt~.SinceΨt~=ΦBt~, from (36) to (37) we have
(38)Tt~=C1TPΦBt~+X1TΦBt~,(39)Tgt~=C2TPΦBt~+X2TΦBt~,which can be written as
(40)Tt~=C1TPΦ+X1TΦBt~=a1,a2,…,am^Bt~,(41)Tgt~=C2TPΦ+X2TΦBt~=a1′,a2′,…,am^′Bt~.(4)
Lete1T=a1,a2,…,am^ and e2T=a1′,a2′,…,am^′; then we have
(42)C1T=e1T−X1TΦPΦ−1,(43)C2T=e2T−X2TΦPΦ−1.By using the disjointness of Block pulse functions, we get [21]
(44)T4t~=a14,a24,…,am^4Bt~=e14TBt~.(5)
Substituting (34), (38), (40), and (44) into (1), we obtain
(45)δtρc24C1TΨt~=−hex⋅C1TPΨt~−hin⋅C1TP−X2T−X1TΨt~−εexσ+εinσe14TBt~+ϖt~,where ϖt~=∑i=13qi+αinG.UsingΨt~=ΦBt~ and (42), we have
(46)δtρc24e1T−X1TΦPΦ−1ΦBt~=−hex⋅e1T−X1TΦPΦ−1PΦBt~−hin⋅e1T−X1TΦPΦ−1P−X2T−X1TΦBt~−εexσ+εinσe14TBt~+ϖt~.Discreting (46) by collocation points, we can get a nonlinear system of algebraic equations for the unknown vector e1T=a1,a2,…,am^ as follows:
(47)δtρc24e1T−X1TΦPΦ−1Φ=−e1T−X1TΦPΦ−1PΦHex−e1T−X1TΦPΦ−1P−X2T−X1TΦHin−εexσ+εinσe14T+ϖT,where
(48)Hex=hext~10⋯00hext~2⋯0⋮⋮⋱⋮00⋯hext~m^,Hin=hint~10⋯00hint~2⋯0⋮⋮⋱⋮00⋯hint~m^,ϖT=ϖt~1,ϖt~2,…,ϖt~m^T.The nonlinear system (47) can be solved by applying the Newton iteration method. Therefore, Tt as the solution of (1) is given by Tt=T24t~=a1,a2,…,am^B24t~.Substituting (35), (40), and (41) into (4), we get
(49)cgmg24C2TΨt~=∫Shine1T−e2TBt~dS.ApplyingΨt~=ΦBt~ and (43), we have
(50)cgmg24e2T−X2TΦPΦ−1ΦBt~=∫Shine1T−e2TBt~dS.Discreting (50) by the same collocation points, we can acquire a linear system of algebraic equations for the unknown vector e2T=a1′,a2′,…,am^′ as follows:
(51)cgmg24e2T−X2TΦPΦ−1Φ=e1T−e2THin′,where
(52)Hin′=S⋅hint~10⋯00S⋅hint~2⋯0⋮⋮⋱⋮00⋯S⋅hint~m^.S is the area of the balloon.Solving this system, we can obtain the approximation of (4).


## 5. Error Analysis

To show the effectiveness of∂T/∂t≈CTΨt, we discuss error analysis of Legendre wavelets. Let ∂Tk,Mt/∂t be the approximation of ∂Tt/∂t, ∂Tk,Mt/∂t=∑n=02k−1∑m=0M−1cnmψnmt. Then, ∂Tt/∂t−∂Tk,Mt/∂t=∑n=2k+∞∑m=M+∞cnmψnmt.Theorem 2.
Suppose that the function∂Tk,Mt/∂t obtained by using Legendre wavelets are the approximation of ∂Tt/∂t, and ∂Tt/∂t is with bounded second derivative; then one has the following estimation.
(53)∂Tt∂t−∂Tk,Mt∂tE≤K25k+6/2Γ′M−1.5ΓM−1.5′′′1/2,where TtE=∫01T2tdt1/2, cnm=∂Tt/∂t,ψnmt, and Γ′t/Γt is double gamma function.Proof. Let ∂Tt/∂t be a function in the interval 0,1 such that
(54)∂3Tt∂t3≤K,
whereK is a positive constant.Using the property∫01ΨtΨtTdt=I (I is the identity matrix), we have
(55)∂Tt∂t−∂Tk,Mt∂tE2=∫01∂Tt∂t−∂Tk,Mt∂t2dt=∫01∑n=2k+∞∑m=M+∞cnmψnmt2dt=∑n=2k+∞∑m=M+∞cnm2∫01ψnm2tdt=∑n=2k+∞∑m=M+∞cnm2,where cnm=∂Tt/∂t,ψnmt=∫01∂Tt/∂t⋅ψnmtdt; then we can obtain
(56)cnm=∫01∂Tt∂tψnmtdt=∫n^−1/2kn^+1/2k∂Tt∂t2m+121/22k/2Pm2kt−n^dt.Let2kt−n^=x; then
(57)cnm=∫−11∂T∂xn^+x2k2m+121/22k/2Pmx12kdx=2m+12k+11/2∫−11∂T∂xn^+x2kPmxdx=12k+12m+11/2∫−11∂T∂xn^+x2kdPm+1x−Pm−1x=12k+12m+11/2∂T∂xn^+x2kPm+1x−Pm−1x−11−12k+12m+11/2∫−11∂2T∂x2n^+x2k12kPm+1x−Pm−1xdx=−123k+12m+11/2∫−11∂2T∂x2n^+x2kPm+1x−Pm−1xdx=−123k+12m+11/2∫−11∂2T∂x2n^+x2kdPm+2x−Pmx2m+3−Pmx−Pm−2x2m−1=−123k+12m+11/2∂2T∂x2n^+x2kPm+2x−Pmx2m+3−Pmx−Pm−2x2m−1−11+125k+12m+11/2∫−11∂3T∂x3n^+x2kPm+2x−Pmx2m+3−Pmx−Pm−2x2m−1dx=125k+12m+11/2∫−11∂3T∂x3n^+x2kPm+2x−Pmx2m+3−Pmx−Pm−2x2m−1dx.Suppose(58)Rx=2m−1Pm+2x−4m+2Pmx+2m+3Pm−2x.Therefore,(59)cnm=125k+12m+11/2∫−11∂3T∂x3n^+x2kPm+2x−Pmx2m+3−Pmx−Pm−2x2m−1dx≤ξ∫−11∂3T∂x3n^+x2kRxdx≤ξK∫−11Rxdx,where ξ=1/25k+12m+11/21/2m+32m−1. Using Cauchy-Schwarz inequality
(60)∫−11Rxdx2≤∫−1112dx∫−112m−12+4m+22+2m+32Pm+22x+Pm2x+Pm−22xdx≤42m−12+4m+22+2m+3212m+5+12m+1+12m−3.Then
(61)∫−11Rxdx≤22m−12+4m+22+2m+321/212m+5+12m+1+12m−31/2.Thus,
(62)cnm≤2Kξη,where η=2m−12+4m+22+2m+321/21/2m+5+1/2m+1+1/2m−31/2.Since(63)ξ2η2=2m−12+4m+22+2m+3225k+12m+12m+322m−1212m+5+12m+1+12m−3≤925k2m+12m−122m−3≤925k2m−34,then
(64)cnm2≤4K2ξ2η2≤36K225k2m−34<36K22n52m−34.Therefore, we have(65)∑n=2k+∞∑m=M+∞cnm2<∑n=2k+∞∑m=M+∞36K22n52m−34=36K2∑n=2k+∞12n5∑m=M+∞12m−34<K225k+6Γ′M−1.5ΓM−1.5′′′.Then we get(66)∂Tt∂t−∂Tk,Mt∂tE2≤K225k+6Γ′M−1.5ΓM−1.5′′′,namely,
(67)∂Tt∂t−∂Tk,Mt∂tE≤K25k+6/2Γ′M−1.5ΓM−1.5′′′1/2.From Theorem2, we can find that ∂Tt/∂t−∂Tk,Mt/∂tE→0 when M is fixed and k→+∞.


## 6. Numerical Implementation of Legendre Wavelet Method for Solving TEE

In order to show the validation of the proposed method, the same stratospheric balloon model [10] at float condition is selected. A spherical balloon with radius R=20m is shown in Figure 4. The film of the balloon is divided into 3018 elements by the software ANSYS 14.0. Other parameters in this part are for εex=εin=αex=αin=0.53, αs=0.12, and ρe=0.35. The surface density is 150 g/m2, and the specific heat is 1500 J/(kg·K). The lifting gas is helium and the wind speed is 10 m/s. The floating altitude is 20 km. The floating latitude and longitude are 40 degrees and 120 degrees, respectively. The balloon was launched during daytime on Spring Equinox 2010.Figure 4
The geometric model of the stratospheric balloon.Figure5 shows the day-night variation of the film element temperature for m^=24 and compares it with the measured data. The degree of the Legendre polynomials is 3. From Figure 5, we can see that the predicted data obtained by our method are in good agreement with measured data [23], which indicates the validation to simulate thermal behavior of the balloon. Due to the solar irradiation, the actual balloon temperature begins to increase before sunrise and after sunset it continues to decrease. The maximum and minimum temperatures are 274 K and 229 K. The variation of the actual balloon temperature is as high as 45 K.Figure 5
The comparison of the temperature of the film.The predicted data of the temperature day-night variation form^=24,32,48,64 are shown in Figure 6. From Figure 6, we can conclude that the temperature of the film varies nonlinearly with time. The reason for this variation is that the solar irradiation appeared at 6 o’clock and vanished at 18 o’clock.Figure 6
The comparison of the temperature of the film for differentm^.The comparison between the predicted data form^=24,64 and the measured data is displayed in Figure 7. Table 1 reveals the CPU time on examples 1–4 for different m^. From Table 1, it is seen that the CPU time on examples 1–4 are less than 1 minute, which implies high efficiency for the method. It can be seen from Figure 7 that the proposed method can predict the thermal behavior of stratospheric balloon effectively, and the simulated results are more credible with m^ increasing. Table 1 reveals the CPU time on simulation for different m^. From Table 1, it is seen that the CPU time are less than 20 seconds, which implies high efficiency for the method.Figure 7
The comparison of the film’s temperature for differentm^=24,64.Table 1
CPU time (in seconds) for differentm^.
CPU time
m
^
=
24
15.881
m
^
=
64
18.254Figure8 shows the comparison of day-night variation of helium temperature obtained by our proposed method and Xia et al.’s [10] method, respectively. From Figure 8, we may find that the maximum and minimum helium temperatures are 262.2 K and 229.1 K, respectively. We can also see that the calculated results are close to Xia et al.’s results by taking a closer look at Figure 8. The effectiveness of the proposed method is demonstrated by the coincidence.Figure 8
The comparison of day-night variation of helium temperature.Comparing Xia et al.’s results with ours, there exist some divergences in Figure8. These are mainly due to the influence of computational errors by using (51). The errors consist of two parts: one is the approximation of the film’s area and the other is the inverse of matrices product. The difference, on the other hand, comes from the number of comparisons.In summary, the main characteristics of the wavelet-based approach which leads to a sparse matrix are (1) the vanishing moments property and (2) having a small interval of support. In fact, the sparseness of the system coefficient and good adaptation in dealing with continuous functions are good advantages of using Legendre wavelets, as shown by numerical example. What is more, the approximate explicit expressions of the temperatures of lifting gas and balloon film are obtained generally, which can calculate the temperatures at any time.


## 7. Conclusion

In the proposed method, we used the properties of the Legendre wavelets to reduce TEE to solve a system of algebraic equations. The temperatures of lifting gas and balloon film will be got by solving the linear and nonlinear system of algebraic equations. The solution is expressed as a truncated Legendre wavelet series and so it can be easily evaluated for arbitrary values of time using any computer program. From the illustrative example, we can conclude that using this approach obtains very satisfactory results. To illustrate the validity and the great potential of the technique, comparisons are made between the predictions obtained by ours and results obtained in previous literature. The proposed method is not only simple but also practical.



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*Source: 7806036-2018-02-08.xml*