Earth’s Energy Balance Model

*Remember to save your work along the way in your IFS space.  If you do not know how to do this ask your GSI.
*Stella is available in the fishbowl and Dana.

Objective
The goal of this class is to gain a working knowledge of, and an insight into, the processes of global change. The natural systems (e.g. ecosystems, climate system) that we would like to understand are extraordinarily complex. To study the response of these systems to change, it is necessary to reduce this complexity. We do this by creating models, simplified representations of reality. Modeling is the process of distilling complex systems down to their essential (and hopefully manageable) components. In this lab, we introduce some of the modeling concepts and tools (STELLA) that we will use throughout the course to study the response of dynamic systems to change.

The Modeling Process
Modeling should be approached in a logical and ordered manner. Though following guidelines may seem tedious and unnecessary at times, it greatly increases the chances that your model will (a) work and (b) be a relatively accurate representation of the actual behavior of a real-life system.

At its essence, modeling is a 5-part process:

1. Define the Problem and the Goals of the Model
This is where most people get into trouble. Aside from programming problems, most models give incorrect results because (a) the system under study was not understood well enough or (b) the modeler did not have a clear idea of what the model was actually supposed to show. Make note of any assumptions needed to simplify the model at this stage.

2. Understand the Real Life System
Figure out the crucial components of the system. (These are represented as stocks, flows, converters and connectors in STELLA.) Exclude any components that are unnecessary. Keep the model as simple as possible, as unnecessary complexity will make it difficult to understand and modify later on.

3. Build the Model
Sketch out the connections between model variables.  Once you have made all of the relevant connections, use STELLA icons to build the model.

4. Test and Revise the Model
Run the model with different data in order to find out if it works, what its limitations are, and where and when it breaks down.

5. Verify the Model
Though not always possible, try to test your model against real world data.
Although we will not be strictly following every step of this guideline in the development of the models in this text, it is important that you keep them in mind as you develop them now and especially in the future.

Create Your First Model
The instructions listed below will guide you through the construction of your first computer model. You may want to refer to the Guide to Basic STELLA Features for help.

To illustrate basic modeling principles and introduce you to STELLA, we will construct a simple model of a typical bathtub. The goal of our modeling is to determine what flow is necessary to fill, but not overfill, our bathtub. Before we proceed with programming our model in STELLA, let’s think about the bathtub system. What is it that we want to describe? What physical laws govern our system? What inputs and outputs are there to our bathtub? What simplifications will we make to our model to make it tractable?

What is it that we want to describe? Because our goal is to fill the bathtub, we want to describe the water volume in the tub. This is our “state variable” that describes the condition of our system, and will have units of m^3.

Most bathtubs have a faucet and a drain. We must include these in our model. Flow from the faucet is the input; flow in to the drain is the output. The flow in will be equal to the rate of flow (m/s) times the area (m^2) of the faucet head. The flow out will be equal to the rate of flow (m/s) times the area (m^2) of the drain. Both of these are volume fluxes, and have units of m3/s.

What physical laws govern our system? The volume of water in the bathtub is dependent upon the amount that comes in and the amount that flows out. We have just described a conservation law. It is this rule that will govern our model. (Strictly speaking, we should be conserving “mass” rather than “volume”. However, because the density of water in to and out of our bathtub is constant, we can make this simplification.) This idea of mass balance will be investigated later in the course.

What simplifications will we make to our model to make it tractable? One simplification is that we will ignore the temperature of the water in our tub. The density of water, that is the number of water molecules per m^3, is temperature dependent. Warm water has a lower density and, as a result, a larger volume than cold water. It turns out that this effect is pretty small and won’t have much consequence on our estimates. What other simplifications are we making?

Now that we have described the rules for our bathtub we can begin constructing it! Follow along with your GSI.

 


Make sure the flow is connected to the stock. If your model, looks like this:

 

 

then the flow was not properly placed within the Bathtub stock.

The question mark in the Faucet flow tool above indicates that an input value is required. Double click on Faucet, and enter an initial value of 0.01, the rate of water flow (m^3/s) from the faucet. Add units!

 

 

 

 

 

!! If you make a mistake, and need to delete an icon or connector, use the dynamite icon, ttp://www.globalchange.umich.edu/globalchange1/current/labs/Lab2_IntroStella/Intro_Stella_clip_image007_0000.gif.  Click and drag the flame of the dynamite icon on top of the offending icon/connector to blow it up. Dynamite is fun, but also permanent! So use caution.

 

 

 

 

 


In the lower left hand corner of the graph, there is a Lock icon. To save the graph and to keep it from getting overwritten by subsequent runs, click on the icon. You can always open a new graph window to plot results from a different experiment.

The STELLA modeling system is a user-friendly interface that allows you to build mathematical equations without getting bogged down in the details of programming and complex math. Take a look at the real workings of the model by clicking on the Equations Tab you see on the extreme left hand side of the screen.  In this equations layer, the icons you created are translated into difference and differential formulas. Although you will not be expected to interpret the math in these equations, you should be able to see what relationships are being represented.

Summary of what we have learned thus far:
So far in this lab exercise we have learned what a model is, and how to construct a simple model in STELLA. In future exercises our models will be more complex, but will follow the general rules learned here.

eit_195s
Objective
The sun radiates energy outward toward the planets, which provides light and heat to the Earth. At the same time, the Earth radiates energy back into space. In this exercise, we will use STELLA to create a model showing these energy flows and the equilibrium that is reached. This model is relatively simple, yet very powerful: it describes the temperature of our planet, one of the key factors that have led to the evolution of life.

 

Figure 1
The sun

Part 1. Define the Problem and Goals of the Model.
The primary goals of this exercise are to illustrate the physical processes that dictate the Earth’s temperature, and to create a model that accurately predicts the radiative equilibrium temperature that maintained the early Earth’s energy balance. It is important that you understand the basic assumptions and conclusions of the model to understand how this process works as a system, so that you can incorporate information learned later on and build on your modeling skills.

Figure 2
Picture of the IR radiation of Earth

Part 2. Understand the Real Life System.
DO NOT START YOUR MODEL UNTIL YOU GET TO THE STEP BY STEP INSTRUCTIONS IN PART 3. Read through the entire Part 2 before you start building the model.

Let’s first consider the stocks and flows that will comprise the heart of our model. The thing that accumulates in our system is energy. So we will represent Earth energy as a stock in our model. The processes affecting this stock are (1) Earth’s capture of solar radiation; and (2) the emission of infrared energy from Earth to space. We will represent these processes by flows into (solar to Earth) and out of (Earth to space) the Earth energy stock (Figure 3).


Figure 3
Initial components of the Earth energy balance model


Figure 4
Solar to Earth

Next, identify the radiation laws (See lecture notes) and other physical properties that govern these flows. We know that the amount of solar radiation reaching the Earth (or any other planet) is a function of its diameter, albedo (ability to reflect radiative energy; this value has no units, can you think of why?), and distance from the sun (solar constant as predicted by the "R-squared Law").

So in our model we will have three converters feeding into the solar to Earth flow: solar constant, Earth albedo and Earth diameter (Figure 4). (Note: diameter is twice the radius)

The equation governing this relationship is:

Equation 1
solar to Earth = solar constant * (1 – Earth albedo) * PI * (Earth diameter / 2) ^2

Similarly, the Stefan-Boltzmann law tells us that the amount of energy emitted by an object goes as the fourth power of its temperature ("E equals sigma T to the fourth"). Therefore, the amount of radiative energy lost from the Earth can be calculated as follows:

Equation 2
Earth to space = PI * (Earth diameter^2) * sigma * (Earth temperature^4)

Thus our model will contain three converters feeding into the Earth to space flow: Earth diameter, sigma, and Earth temperature, where sigma represents the constant in the Stefan-Boltzmann equation (Figure 5).


Figure 5
Earth to space

Finally, the first law of thermodynamics tells us that a body’s temperature is given by its energy divided by its heat capacity:

Equation 3
Earth temperature = Earth energy / heat capacity

And, given that the surface of the "blue planet" is primarily comprised of water, we can use the properties of water to calculate the Earth’s heat capacity (by making the simplifying assumption that the Earth is covered by a uniform layer of water.)

Equation 4
heat capacity = PI * (Earth diameter^2) * water depth * density of water * specific heat of water

So our final model should look equivalent Figure 6 below (do not try to simply copy Figure 6, it will not work, go through the directions step by step):

Figure 6
Complete model structure

Part 3. Build the Model.

Units

J = Joule

s = second

m = meter

yr = year

K = degrees Kelvin

kg = kilogram

1. Start up STELLA.

2. To get into modeling mode, click once on the “Model” tab on the left hand side of your screen. You are now ready to start modeling. Note: in this model, all units are written out within "curly" brackets: {}. The units entered inside the curly brackets are notes that are not read by STELLA but allow you to keep track of your units. You may also use the units button to enter them, or simply type the units out exactly as they are in the lab, including the brackets.

3. Create the Earth energy stock by clicking on the stock icon and then on the screen. To name the stock: type Earth energy in to the highlighted text area. Then double-click on the question mark to set the initial value. Type 0.00 in the dialog box and click OK. This allows us to watch the Earth warm up from its initial temperature, which in this model is absolute zero {K}.

4. Create a flow into the Earth energy stock. (Click on the flow icon , place the pointer to the left of Earth energy, and by dragging the mouse, join the flow to the stock. Make sure there is only one "cloud" attached to the flow icon.) Name the flow solar to Earth.

5. Now create another flow out of the Earth energy stock and name it Earth to space. (Click on the flow icon, place the pointer inside the stock and drag the mouse outside of the box. Again, make sure there is only one "cloud" attached to the flow icon.) At this point your model should look like Figure 3.

6. We will now add a number of converters to the model, each of which will contain one of the constants needed for our simulation.

7. Click on the converter icon , place it near the solar to Earth, and name this first converter solar constant. Double-click on the question mark, type in 1368 {J/(m^2 * s)} * 3.15576E7 {seconds per year} as the value, and click OK. (3.15576E7 is used to express 3.15576 x 107, the scientific notation for 31, 557, 600.

8. Create two more converters named Earth albedo and Earth diameter.  Define the values of Earth albedo and Earth diameter to be 0.30 and 12742E3 {m} respectively.

9. Now connect the converters, one by one, to the solar-to-Earth flow using the red connectors. Do this by clicking on the connector icon , placing the pointer on the boundary of the converter and connecting it to solar to Earth. The left side of your model should look like Figure 4.

10. Repeat step 6 to add a converter below the Earth to space flow called sigma (Stefan-Boltzmann constant). Once again use the connector tool to connect sigma to Earth to space, and set the value of this constant equal to 5.67E-8 {J/(m^2 * s * K^4)} * 3.15576E7 {seconds per year}.

11. To add a second Earth diameter converter near Earth to space, we will need to use a ghost icon  to indicate that it is the same constant used on the left side of the model. Ghost icons are used primarily for aesthetic purposes, to improve the legibility and comprehensibility of a model (avoiding the "spaghetti" that accumulates when there are too many connectors criss-crossing each other).

Click on the ghost icon , and then on the original Earth diameter converter. Then click near Earth to space to add another copy of this converter to the model. (The ghost converter should look shadowy, with a dotted outline.) Connect it to Earth to space. The value of this converter should already be set.

12. Create another converter named Earth temperature below the Earth energy stock to represent the radiation equilibrium temperature of the planet. Insert one connector from Earth temperature to Earth to space, and another from Earth energy to Earth temperature (since temperature depends on energy)

13. Before we can define Earth temperature, we must add heat capacity to the model. Create another converter below Earth temperature and name it heat capacity. Insert a connector from heat capacity to Earth temperature.

14. Now we will add the converters that are needed to define heat capacity. Add three more converters named water depth, specific heat of water and density of water, and connect them one by one to heat capacity. Set the values of these constants to 1.0 {m}, 4218 {J/(kg * K)} and 1000 {kg/m^3}, respectively.

15. Finally, repeat step 11 to add another ghost converter for Earth diameter and then connect it to heat capacity.

16. Now we are ready to input equations. Double-click on the heat capacity icon and use Equation 4 to define the value of this converter:

PI can be found in the "builtins" list on the right side of the dialog box. (Make sure to use the list of required inputs to enter variable names, rather than typing them manually. STELLA will not accept variable names that do not match exactly.)

PI*(Earth_diameter^2)*water_depth*density_of_water* specific_heat_of _water.

17. Repeat step 16 for the Earth temperature converter, using Equation 3. Then use Equations 1 and 2 to define the solar to Earth and Earth to space flows, respectively.
All done! Your model should now look like Figure 6.

Part 4. Test the Model
Now run the model with initial Earth energy of zero. We are interested in observing the change over time in Earth energy, Earth temperature and Earth to space.

Insert a numeric display box on your workspace above your model using the  numeric display icon. This will allow you to see the numeric value of a certain variable at the end of the simulation. Double-click on your empty numeric display box and select Earth temperature. Click on >> and make sure "retain ending value" is selected, and leave other options at the default settings.

To view the model output, click on the graph icon and then click on the screen to bring up a graph window, which will not yet have a legend on the y-axis. Double-click on the graph to select which variables to show. Select Earth energy, Earth temperature, and Earth to space by highlighting them in the allowable column and then moving them to the selected column by clicking on >>. In the space for the title, enter "Earth Energy Balance." Click OK to close the dialog box.

 

To run and plot the graph, select run specs from the run menu. In the dialog box that appears, input the length of the simulation (from 0 to 1.00), time step (DT = .01) and unit of time (years). These parameters mean that we are modeling the change in the Earth’s energy balance over a period of one year, in increments of 1/100 year. Click OK to return. Select run from the run menu on top of the screen to execute the model.

Figure 7
Graph of Earth’s energy, Earth’s temperature and Earth to space radiation

Looking at the output graph, we see that the model in the equilibrium region predicts a radiative equilibrium temperature of 255 K (-18C). This is the temperature that results in a balance between radiation received by the sun and infrared emissions from the Earth.

You will also notice that the curves for Earth energy (1) and Earth temperature (2) have the same shape. This happens here because the two variables are in direct proportion to one another (although the actual values are different, as illustrated by the scales shown along the Y-axis). The Earth to space (3) curve has a different shape because it is proportional to the fourth power of Earth temperature (T^4). When T is small, relative to its maximum value, the T^4 is very, very small as shown on the lower left corner of the graph; as the two variables approach their maximum values, Earth to space catches up with Earth temperature and they both attain their equilibrium values. (The Y-axis scales for Earth energy and Earth to space show zeros trailing of the chart because STELLA is trying to display all the variables in the same numerical units (i.e. not scientific notation).

Units

J = Joule

s = second

m = meter

yr = year

K = degrees Kelvin

kg = kilogram

Table 1
Model units and abbreviations

 

Part 5: Explore the Model  

         For your assignment you will be turning in a Word document on CTools. Include a screenshot of your model structure so far, copy and paste your graph, and the equations (located under the “Equation” tab) from your EBM into your Word document. Then answer the following questions, also in your Word document.

Question 1
     Take a step back and think about the system we are modeling. To model this system we have made many assumptions. For instance, we assume that the Earth’s surface is covered by 1 meter of water. As you are probably aware, this simply isn’t true…but the assumption allows us to simplify the system. Along this same vein, think about other assumptions we have made in this model, list three of these assumptions and explain how such an assumption may affect the model’s output. Were these assumptions reasonable?

 Question 2
          If you model a different planet, either closer or further from the sun, than planet   Earth, is the value of the solar constant the same? Why or why not and how does it change? Finally, do you need to change the structure of the model to reflect the change in the solar constant?

 

Part 6: Explore the Solar System

Save the Earth model you created above as “Earth model”. Next save a second copy of the exact same model, just re-name it the "Venus model". Now we’ll adjust the ‘Venus model’ to predict the temperature of Venus. We will assume the same heat capacity as in the Earth model, but we will use the Venus diameter shown in Table 2. **Pay attention to the units (Think: What unit did we originally use for the Earth's diameter?).** Finally, there are two other inputs that need to be modified: Venus albedo and the solar constant (keep reading to figure out how).

Remember that the value for the solar constant that we used in the Earth model was adjusted for the Earth’s distance from the sun. We can re-adjust this for Venus’ distance from the sun by multiplying the function we used by the ratio of each planet’s distance from the sun [Dist2earth/Dist2venus], which is the ratio of Earth’s distance from the sun squared to Venus’ distance from the sun squared (refer to Table 2). The value to be used for Venus albedo can be obtained from the Internet or another reference source (you may use either the integral or visual albedo). Be sure to cite your source in your homework.

 

 

Diameter
(km)

Distance
from Sun
(106 km)

surface
temperature
(oC)

surface
temperature
(K)

Density
g/cm3

Main 
atmospheric
constituents

Sun

1,392 x 103

-

5,527

 5,800

 

-

Mercury

4,880

58

260

533

5.4 (rocky)

-

Venus

12,112

108

480

753

5.3 (rocky)

CO2

Earth

12,742

150

15

288

5.5 (rocky)

N2, O2

Mars

6,800

228

-60

213

3.9 (rocky)

CO2

Jupiter

143,000

778

-110

163

1.3 (icy)

H2, He

Saturn

121,000

1,427

-190

83

0.7 (icy)

H2, He

Uranus

52,800

2,869

-215

58

1.3 (icy)

H2, CH4

Neptune

49, 000

4,498

-225

48

1.7 (icy)

H2, CH4

Pluto

3,100

5,900

-235

38

?

CH4

Table 2
Properties of the Planets (note that the units may not match those used in the model)
**You will need to do a unit conversion!**

 

Question 3
     Again paste a screenshot of your new model structure, the graph, and the equations for your Venus model into your Word document.   What value does the model predict for the radiative equilibrium temperature of Venus? (Don't forget to cite your source for Venus' albedo, and include the number you found in your Word document.)

 

Question 4
     Compare the outputs of the Venus and the Earth model. Even though Venus is closer to the sun, it has a lower predicted temperature, why?   


Figure 8
A comparison of Earth (on the right) and Venus

Question 5
The radiative equilibrium temperature predicted in our Earth model differs from the actual surface temperature of today’s Earth (~300 K) by ~40K. Our Venus model differed from the actual surface temperature of today’s Venus by >400K. Why does our model miscalculate the actual temperatures? What accounts for the large discrepancy between Earth’s and Venus’ surface temperatures and the models’ prediction? 

*If you're interested in learning more about the topic, feel free to try the Virtual Global Warming Activity.

By the beginning of class next week, please turn in your Word document through the assignments page on your section CTools site. Your Word document should contain:

Sources
The image at the top of this page is from NASA's Solar and Heliospheric Observatory
http://photojournal.jpl.nasa.gov/jpegMod/PIA00112_modest.jpg
http://wikyonos.seos.uvic.ca/climate-lab/front_page_pics/temperature.lrg.jpeg