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The '''Grashof number''' ('''Gr''') is a [[dimensionless number]] in [[fluid dynamics]] and [[heat transfer]] which approximates the ratio of the [[buoyancy]] to [[viscous]] force acting on a fluid. It frequently arises in the study of situations involving [[natural convection]]. It is named after the German engineer [[Franz Grashof]].
 
:<math> \mathrm{Gr}_L = \frac{g \beta (T_s - T_\infty ) L^3}{\nu ^2}\, </math> for vertical flat plates
 
:<math> \mathrm{Gr}_D = \frac{g \beta (T_s - T_\infty ) D^3}{\nu ^2}\, </math> for pipes
:<math> \mathrm{Gr}_D = \frac{g \beta (T_s - T_\infty ) D^3}{\nu ^2}\, </math> for bluff bodies
 
where the ''L'' and ''D'' subscripts indicates the length scale basis for the Grashof Number.
 
: ''g''  = [[standard gravity|acceleration due to Earth's gravity]]
: ''&beta;'' = [[coefficient of thermal expansion|volumetric thermal expansion coefficient]] (equal to approximately 1/''T'', for ideal fluids, where ''T'' is absolute temperature)
: ''T''<sub>''s''</sub> = surface temperature
: ''T''<sub>''∞''</sub> = bulk temperature
: ''L'' = characteristic length
: ''D'' = diameter
: ''&nu;'' = [[kinematic viscosity]]
 
The transition to turbulent flow occurs in the range <math>10^8 < \mathrm{Gr}_L < 10^9</math> for natural convection from vertical flat plates. At higher Grashof numbers, the boundary layer is turbulent; at lower Grashof numbers, the boundary layer is laminar.
 
The product of the Grashof number and the [[Prandtl number]] gives the [[Rayleigh number]], a dimensionless number that characterizes convection problems in heat transfer.
 
There is an analogous form of the '''Grashof number''' used in cases of natural convection [[mass transfer]] problems.
 
:<math> \mathrm{Gr}_c = \frac{g \beta^* (C_{a,s} - C_{a,a} ) L^3}{\nu^2}</math>
 
where
 
:<math> \beta^* = -\frac{1}{\rho} \left ( \frac{\partial \rho}{\partial C_a} \right )_{T,p}</math>
 
and
 
: ''g''  = [[standard gravity|acceleration due to Earth's gravity]]
: ''C''<sub>''a,s''</sub> = concentration of species ''a'' at surface
: ''C''<sub>''a,a''</sub> = concentration of species ''a'' in ambient medium
: ''L'' = characteristic length
: ''&nu;'' = kinematic viscosity
: ''&rho;'' = [[fluid]] [[density]]
: ''C''<sub>''a''</sub> = concentration of species ''a''
: ''T'' = constant temperature
: ''p'' = constant pressure
<!-- : ''Q'' = Helmet Pleasure Ratio -->
 
==Derivation of Grashof Number==
The first step to deriving the '''Grashof number''' is manipulating the volume expansion coefficient, '''<math>\mathrm{\beta}</math>''' as follows:
 
:<math>\beta = \frac{1}{v}\left(\frac{\partial v}{\partial T}\right)_p =\frac{-1}{\rho}\left(\frac{\partial\rho}{\partial T}\right)_p</math>
 
It should be noted that the <math>v</math> in the equation above, which represents [[specific volume]], is not the same as the <math>v</math> in the subsequent sections of this derivation, which will represent a velocity.  This partial relation of the volume expansion coefficient, '''<math>\mathrm{\beta}</math>''', with respect to fluid density, '''<math>\mathrm{\rho}</math>''', given constant pressure, can be rewritten as
 
:<math>\rho=\rho_o (1-\beta \Delta T)</math>
 
where
 
:<math>\rho_o</math> - bulk fluid density
 
:<math>\rho</math> - boundary layer density
 
:<math>\Delta T = (T - T_o)</math> - temperature difference between boundary layer and bulk fluid
 
There are two different ways to find the '''Grashof Number''' from this point. One involves the energy equation while the other incorporates the buoyant force due to the difference in density between the boundary layer and bulk fluid.
 
=== Energy Equation ===
This discussion involving the energy equation is with respect to rotationally symmetric flow. This analysis will take into consideration the effect of gravitational acceleration on flow and heat transfer. The mathematical equations to follow apply both to rotational symmetric flow as well as two-dimensional planar flow.
 
:<math>\frac{\partial}{\partial s}(\rho u r_o^{n})+{\frac{\partial}{\partial y}}(\rho v r_o^{n})=0</math>
 
where
 
:<math>s</math> = rotational direction, i.e. direction parallel to the surface
:<math>u</math> = tangential velocity, i.e. velocity parallel to the surface
:<math>y</math> = planar direction, i.e. direction normal to the surface
:<math>v</math> = normal velocity, i.e. velocity normal to the surface
:<math>r_o</math> = radius
 
In this equation the superscript n is to differentiate between rotationally symmetric flow from planar flow. The following characteristics of this equation hold true.
 
:<math>n</math> = 1 - rotationally symmetric flow
:<math>n</math> = 0 - planar, two-dimensional flow
:<math>g</math> - gravitational acceleration
 
This equation expands to the following with the addition of physical fluid properties:
 
:<math>\rho\left(u \frac{\partial u}{\partial s} + v \frac{\partial u}{\partial y}\right) = \frac{\partial}{\partial y}\left(\mu \frac{\partial u}{\partial y}\right) - \frac{d p}{d s} + \rho g</math>
 
From here we can further simplify the momentum equation by setting the bulk fluid velocity to 0 (''u'' = 0).
 
:<math>\frac{d p}{d s}=\rho_o g</math>
 
This relation shows that the pressure gradient is simply a product of the bulk fluid density and the gravitational acceleration. The next step is to plug in the pressure gradient into the momentum equation.
 
:<math>\rho\left(u \frac{\partial u}{\partial s}+v \frac{\partial u}{\partial y}\right)=\mu \left(\frac{\partial^2 u}{\partial y^2}\right)+\rho g \beta (T-T_o)</math>
 
Further simplification of the momentum equation comes by substituting the volume expansion coefficient, density relationship <math>\rho_o - \rho = \beta \rho(T - T_o)</math>, found above, and kinematic viscosity relationship, <math>\nu = \frac{\mu}{\rho}</math>, into the momentum equation.
 
:<math> u\left(\frac{\partial u}{\partial s}\right)+v \left(\frac{\partial v}{\partial y}\right)=\nu \left(\frac{\partial^2 u}{\partial y^2}\right)+g \beta(T - T_o)</math>.
 
To find the Grashof Number from this point, the preceding equation must be non-dimensionalized. This means that every variable in the equation should have no dimension and should instead be a ratio characteristic to the geometry and setup of the problem. This is done by dividing each variable by corresponding constant quantities. Lengths are divided by a characteristic length, <math>L_c</math>. Velocities are divided by appropriate reference velocities, <math>V</math>, which, considering the Reynolds number, gives <math>V=\frac{\mathrm{Re}_L \nu}{L_c}</math>. Temperatures are divided by the appropriate temperature difference, <math>(T_s - T_o)</math>. These dimensionless parameters look like the following:
 
:<math>s^*=\frac{s}{L_c}</math>,
   
:<math>y^* =\frac{y}{L_c}</math>,
 
:<math>u^*=\frac{u}{V}</math>,   
 
:<math>v^* = \frac{v}{V}</math>,   
 
:<math>T^*=\frac{(T-T_o)}{(T_s - T_o)}</math>.
 
The asterisks represent dimensionless parameter. Combining these dimensionless equations with the momentum equations gives the following simplified equation.
 
:<math>u^* \frac{\partial u^*}{\partial s^*} + v^* \frac{\partial u^*}{\partial y^*} =\left[ \frac{g \beta(T_s - T_o)L_c^{3}}{\nu^2} \right] \frac{T^*}{\mathrm{Re}_L^{2}}+\frac{1}{\mathrm{Re}_L} \frac{\partial^2 u^*}{\partial {y^*}^2}</math>
 
where
 
:<math>T_s</math> - surface temperature
 
:<math>T_o</math> - bulk fluid temperature
 
:<math>L_c</math> - characteristic length
 
The dimensionless parameter enclosed in the brackets in the preceding equation is known as the '''Grashof Number'''
 
:<math>\mathrm{Gr}=\frac{g \beta(T_s-T_o)L_c^{3}}{\nu^2}</math>
 
===Buckingham Pi Theorem===
Another form of dimensional analysis that will result in the '''Grashof Number''' is known as the [[Buckingham Pi theorem]]. This method takes into account the buoyancy force per unit volume, <math>F_b</math> due to the density difference in the boundary layer and the bulk fluid.
 
<math>F_b = (\rho - \rho_o) g</math>
This equation can be manipulated to give,
 
<math>F_b = \beta g \rho_o \Delta T</math>
 
The list of variables that are used in the Buckingham Pi method is listed below, along with their symbols and dimensions.
 
{| class="wikitable"
|-
! Variable
! Symbol
! Dimensions
|-
| Significant Length
| <math>L</math>
| <math>\mathrm{L}</math>
|-
| Fluid Viscosity
| <math>\mu</math>
| <math>\mathrm{\frac{M}{L t}}</math>
|-
| Fluid Heat Capacity
| <math>c_p</math>
| <math>\mathrm{\frac{Q}{M T}}</math>
|-
| Fluid Thermal Conductivity
| <math>k</math>
| <math>\mathrm{\frac{Q}{L t T}}</math>
|-
| Volume Expansion Coefficient
| <math>\beta</math>
| <math>\mathrm{\frac{1}{T}}</math>
|-
| Gravitational Acceleration
| <math>g</math>
| <math>\mathrm{\frac{L}{t^2}}</math>
|-
| Temperature Difference
| <math>\Delta T</math>
| <math>\mathrm{T}</math>
|-
| Heat Transfer Coefficient
| <math>h</math>
| <math>\mathrm{\frac{Q}{L^2 t T}}</math>
|}
 
With reference to the [[Buckingham Pi Theorem]] there are 9 – 5 = 4 dimensionless groups. Choose ''L'', <math>\mu,</math> ''k'', ''g'' and <math>\beta</math> as the reference variables. Thus the <math>\pi</math> groups are as follows:
 
<math>\pi_1 = L^a \mu^b k^c \beta^d g^e c_p</math>,
 
<math>\pi_2 = L^f \mu^g k^h \beta^i g^j \rho</math>,
 
<math> \pi_3 = L^k \mu^l k^m \beta^n g^o \Delta T</math>,
 
<math> \pi_4 = L^q \mu^r k^s \beta^t g^u h</math>.
 
Solving these <math>\pi </math> groups gives:
 
<math> \pi_1 = \frac{\mu(c_p)}{k} = Pr</math>,
 
<math> \pi_2 =\frac{l^3 g \rho^2}{\mu^2}</math>,  
 
<math> \pi_3 =\beta \Delta T</math>,
 
<math> \pi_4 =\frac{h L}{k} = Nu</math>
 
From the two groups <math>\pi_2</math> and <math>\pi_3,</math> the product forms the '''Grashof Number'''
 
:<math>\pi_2 \pi_3=\frac{\beta g \rho^2 \Delta T L^3}{\mu^2} = \mathrm{Gr}</math>
 
Taking <math>\nu = \frac{\mu}{\rho}</math> and <math>\Delta T = (T_s - T_o)</math> the preceding equation can be rendered as the same result from deriving the '''Grashof Number''' from the energy equation.
 
<math>\mathrm{Gr} = \frac{\beta g \Delta T L^3}{\nu^2}</math>
 
In forced convection the '''[[Reynolds Number]]''' governs the fluid flow. But, in natural convection the '''Grashof Number''' is the dimensionless parameter that governs the fluid flow. Using the energy equation and the buoyant force combined with dimensional analysis provides two different ways to derive the '''Grashof Number'''.
 
==References==
<div class="references-small">
* Jaluria, Yogesh. ''Natural Convection Heat and Mass Transfer'' (New York: Pergamon Press, 1980).
</div>
 
<div class="references-small">
* Cengel, Yunus A. ''Heat and Mass Transfer: A Practical Approach, 3rd Edition'' (Boston: McGraw Hill, 2003).
</div>
 
<div class="references-small">
* [[Ernst R. G. Eckert|Eckert, Ernst R. G.]] and Drake, Robert M. ''Analysis of Heat and Mass Transfer'' (New York: McGraw Hill, 1972).
</div>
 
<div class="references-small">
* Welty, James R. ''Fundamentals of Momentum, Heat, and Mass Transfer'' (New York: John Wiley & Sons, 1976).
</div>
 
{{NonDimFluMech}}
 
{{DEFAULTSORT:Grashof Number}}
[[Category:Convection]]
[[Category:Dimensionless numbers of fluid mechanics]]
[[Category:Dimensionless numbers of thermodynamics]]
[[Category:Fluid dynamics]]
[[Category:Heat transfer]]
[[Category:Buoyancy]]

Revision as of 22:30, 11 October 2013

The Grashof number (Gr) is a dimensionless number in fluid dynamics and heat transfer which approximates the ratio of the buoyancy to viscous force acting on a fluid. It frequently arises in the study of situations involving natural convection. It is named after the German engineer Franz Grashof.

GrL=gβ(TsT)L3ν2 for vertical flat plates
GrD=gβ(TsT)D3ν2 for pipes
GrD=gβ(TsT)D3ν2 for bluff bodies

where the L and D subscripts indicates the length scale basis for the Grashof Number.

g = acceleration due to Earth's gravity
β = volumetric thermal expansion coefficient (equal to approximately 1/T, for ideal fluids, where T is absolute temperature)
Ts = surface temperature
T = bulk temperature
L = characteristic length
D = diameter
ν = kinematic viscosity

The transition to turbulent flow occurs in the range 108<GrL<109 for natural convection from vertical flat plates. At higher Grashof numbers, the boundary layer is turbulent; at lower Grashof numbers, the boundary layer is laminar.

The product of the Grashof number and the Prandtl number gives the Rayleigh number, a dimensionless number that characterizes convection problems in heat transfer.

There is an analogous form of the Grashof number used in cases of natural convection mass transfer problems.

Grc=gβ*(Ca,sCa,a)L3ν2

where

β*=1ρ(ρCa)T,p

and

g = acceleration due to Earth's gravity
Ca,s = concentration of species a at surface
Ca,a = concentration of species a in ambient medium
L = characteristic length
ν = kinematic viscosity
ρ = fluid density
Ca = concentration of species a
T = constant temperature
p = constant pressure

Derivation of Grashof Number

The first step to deriving the Grashof number is manipulating the volume expansion coefficient, β as follows:

β=1v(vT)p=1ρ(ρT)p

It should be noted that the v in the equation above, which represents specific volume, is not the same as the v in the subsequent sections of this derivation, which will represent a velocity. This partial relation of the volume expansion coefficient, β, with respect to fluid density, ρ, given constant pressure, can be rewritten as

ρ=ρo(1βΔT)

where

ρo - bulk fluid density
ρ - boundary layer density
ΔT=(TTo) - temperature difference between boundary layer and bulk fluid

There are two different ways to find the Grashof Number from this point. One involves the energy equation while the other incorporates the buoyant force due to the difference in density between the boundary layer and bulk fluid.

Energy Equation

This discussion involving the energy equation is with respect to rotationally symmetric flow. This analysis will take into consideration the effect of gravitational acceleration on flow and heat transfer. The mathematical equations to follow apply both to rotational symmetric flow as well as two-dimensional planar flow.

s(ρuron)+y(ρvron)=0

where

s = rotational direction, i.e. direction parallel to the surface
u = tangential velocity, i.e. velocity parallel to the surface
y = planar direction, i.e. direction normal to the surface
v = normal velocity, i.e. velocity normal to the surface
ro = radius

In this equation the superscript n is to differentiate between rotationally symmetric flow from planar flow. The following characteristics of this equation hold true.

n = 1 - rotationally symmetric flow
n = 0 - planar, two-dimensional flow
g - gravitational acceleration

This equation expands to the following with the addition of physical fluid properties:

ρ(uus+vuy)=y(μuy)dpds+ρg

From here we can further simplify the momentum equation by setting the bulk fluid velocity to 0 (u = 0).

dpds=ρog

This relation shows that the pressure gradient is simply a product of the bulk fluid density and the gravitational acceleration. The next step is to plug in the pressure gradient into the momentum equation.

ρ(uus+vuy)=μ(2uy2)+ρgβ(TTo)

Further simplification of the momentum equation comes by substituting the volume expansion coefficient, density relationship ρoρ=βρ(TTo), found above, and kinematic viscosity relationship, ν=μρ, into the momentum equation.

u(us)+v(vy)=ν(2uy2)+gβ(TTo).

To find the Grashof Number from this point, the preceding equation must be non-dimensionalized. This means that every variable in the equation should have no dimension and should instead be a ratio characteristic to the geometry and setup of the problem. This is done by dividing each variable by corresponding constant quantities. Lengths are divided by a characteristic length, Lc. Velocities are divided by appropriate reference velocities, V, which, considering the Reynolds number, gives V=ReLνLc. Temperatures are divided by the appropriate temperature difference, (TsTo). These dimensionless parameters look like the following:

s*=sLc,
y*=yLc,
u*=uV,
v*=vV,
T*=(TTo)(TsTo).

The asterisks represent dimensionless parameter. Combining these dimensionless equations with the momentum equations gives the following simplified equation.

u*u*s*+v*u*y*=[gβ(TsTo)Lc3ν2]T*ReL2+1ReL2u*y*2

where

Ts - surface temperature
To - bulk fluid temperature
Lc - characteristic length

The dimensionless parameter enclosed in the brackets in the preceding equation is known as the Grashof Number

Gr=gβ(TsTo)Lc3ν2

Buckingham Pi Theorem

Another form of dimensional analysis that will result in the Grashof Number is known as the Buckingham Pi theorem. This method takes into account the buoyancy force per unit volume, Fb due to the density difference in the boundary layer and the bulk fluid.

Fb=(ρρo)g This equation can be manipulated to give,

Fb=βgρoΔT

The list of variables that are used in the Buckingham Pi method is listed below, along with their symbols and dimensions.

Variable Symbol Dimensions
Significant Length L L
Fluid Viscosity μ MLt
Fluid Heat Capacity cp QMT
Fluid Thermal Conductivity k QLtT
Volume Expansion Coefficient β 1T
Gravitational Acceleration g Lt2
Temperature Difference ΔT T
Heat Transfer Coefficient h QL2tT

With reference to the Buckingham Pi Theorem there are 9 – 5 = 4 dimensionless groups. Choose L, μ, k, g and β as the reference variables. Thus the π groups are as follows:

π1=Laμbkcβdgecp,

π2=Lfμgkhβigjρ,

π3=LkμlkmβngoΔT,

π4=Lqμrksβtguh.

Solving these π groups gives:

π1=μ(cp)k=Pr,

π2=l3gρ2μ2,

π3=βΔT,

π4=hLk=Nu

From the two groups π2 and π3, the product forms the Grashof Number

π2π3=βgρ2ΔTL3μ2=Gr

Taking ν=μρ and ΔT=(TsTo) the preceding equation can be rendered as the same result from deriving the Grashof Number from the energy equation.

Gr=βgΔTL3ν2

In forced convection the Reynolds Number governs the fluid flow. But, in natural convection the Grashof Number is the dimensionless parameter that governs the fluid flow. Using the energy equation and the buoyant force combined with dimensional analysis provides two different ways to derive the Grashof Number.

References

  • Jaluria, Yogesh. Natural Convection Heat and Mass Transfer (New York: Pergamon Press, 1980).
  • Cengel, Yunus A. Heat and Mass Transfer: A Practical Approach, 3rd Edition (Boston: McGraw Hill, 2003).
  • Eckert, Ernst R. G. and Drake, Robert M. Analysis of Heat and Mass Transfer (New York: McGraw Hill, 1972).
  • Welty, James R. Fundamentals of Momentum, Heat, and Mass Transfer (New York: John Wiley & Sons, 1976).

Template:NonDimFluMech