Showing posts with label modelling. Show all posts
Showing posts with label modelling. Show all posts

19 January 2016

The Pacemaker of the Chandler Wobble

Abstract: The Chandler Wobble is one of the largest circumannual periodic or quasi-periodic variations in the earth's orientation.  After over a century of searching for its forcing, it was found to be caused by atmospheric circulation and induced ocean circulation and pressure.  The question of why there should be such forcing from the atmosphere has remained open. I suggest that variations in earth-sun distance cause this forcing to the atmosphere and thence the ocean.  Analysis of earth-sun distance, earth's orientation, and atmospheric winds shows a coherent relationship between the atmosphere and earth orientation at just those periods expected from earth-sun distance variation.  As this is a general mechanism, it can be used in examining regular climatic variations on a wide range of periods and for climate parameters other than the earth's orientation.

-- -- -- -- -- -- -- 

That is the abstract for the paper I link to below.  It's not a peer-reviewed paper in the sense of being in a peer-reviewed journal.   But it has been reviewed by an expert in the field (William P. O'Connor), who was quite favorable.

I am posting the idea and paper here.  Long past time for the ideas to be discussed.  If they're shredded in the blogosphere, so be it.  I have quite a bit more than what I've put in the document. Over the next few days and weeks, I'll post more of those additional materials as well.

The Pacemaker of the Chandler Wobble, Grumbine 2014

02 June 2015

How to build a climate model?

How is it that we go about building climate models?  One thing is, that we would like to build our model to represent everything that we know happens.  If we could actually do so -- mainly meaning if the computers were fast enough -- life would be simple.  As usual, life is not simple.

I'll take one feature as a poster child.  We know the laws of motion pretty well.  I could write them down pretty easily and with only a moderate amount more effort write a computer program to solve them.  These are the Navier-Stokes equations.  On one hand, they're surprisingly complex (from them comes dynamical chaos), but on the other, they're no problem -- we know how to write the computer programs to do conservation of momentum.  Ok entire books have been written on even a single portion of the problem.  Still, the books have already been written.

The problem is, if you want to run your climate model using what we know is a representation sufficient to capture everything we need to do, in order to represent everything we know is going on, you need to have your grid points only 1 millimeter apart.  That's ok, but it means something like 10^30 times as much computing power as the world's most powerful computer today. (A million trillion trillion times as much computing power.)

What do we do in the mean time?

01 June 2015

What is a model?

In the blogospheric talk about climate change 'model' gets mentioned a lot.  Sometimes it's merely descriptive, and often it is perjorative.  But it is mostly never really defined.  Like or loath them, nobody says just what models are.  Except for me, here and now.  (And probably a number of other people at other times and places -- but still, few and far between. :-)

'Obviously' a model is a particularly attractive human.  Right?  I've actually received email at my workplace (a 'modelling branch') from people who were trying to advance the careers of their models, in this sense of model.  We don't deal with that kind of model.

'Obviously' a model is to take the original (the Apollo Saturn V rocket that took people to the moon, for example) and duplicate everything about it, but at 1/32 the original size  Right?  Perhaps.  I know people tho like this sort of thing.  But again that's not what we mean either if we are discussing climate (or atmosphere, ocean, sea ice, land, glacier, ...) models.

For my purposes, a model is an idealized, and/or simplified, representation of the real world.  When we are interested in something as big and complex as climate, or even just the Arctic sea ice pack, we really can't cope with the whole thing in all of its glorious complexity.  We have to simplify the reality somehow.  That simplification is the model.

In this sense of 'model', models are everywhere.  We use a model for human behavior when we decide what somebody else means when they raise their hand in a certain way.  (is it open hand, or a fist?  did they just say 'hello', or 'I'm going to kill you'.  and so on)  Weather has also been modelled by using 'dishpans' -- Raymond Hide and David Fultz being two of the best examples of people taking this approach*.

03 June 2013

Building a climate model

Last Friday I mentioned a model, and will be getting to how it connects to Saturn's hurricane.  But some interesting to you, I hope, byways occurred to me. 

Let's start with the notion of a model.  Sometimes people quote sarcastically George Box's observation "All models are wrong.  Some models are useful."  Often they omit the second half.  And often they ignore the fact, well-known to any observationalist, that the same applies to observations. 

Models are idealizations of the real thing.  As an idealization, they don't represent reality fully.  This is mandatory for my kind of models.  Suppose you want to model ice ages, which span 100,000s of years.  A complete, non-idealized, model would be exactly an entire duplicate Earth, in a duplicate solar system, that we could control for our experiments.  Which might be fine as far as that goes, but would also mean we'd have to wait 100,000 years to see the result of 1 ice age experiment.  'Real time' modeling doesn't cut it for climate.  Or for weather -- if it takes 24 hours to make a 24 hour forecast of the weather, you really can't get much use from the model.

Being able to get an approximate answer much faster than real time is crucial to weather and climate modeling.  I backed in to this by way of some computer sciency experimentation I was doing.  Consider the important element being how much faster that you can get an answer than in real time -- how much 'lead' you can get.  One figure of merit, for instance, is to get a 24 hour model forecast or 'run' in only 1 hour.  This gives you 23 hours to make use of the model before the weather hits.  Obviously the more powerful the computer, the more computing you can do in 1 hour.  But this runs in to some other issues.

22 March 2012

Technical followup on the simplest climate model

Tuesday I took up reconsidering the simplest climate model.  This time, I'm trying to get rid of the annoying bit of having to know the planet's albedo (reflectivity) in order to find its temperature.  Instead, to have some fundamental relationship between temperature and albedo, so that everything in the model is either a fundamental constant (the Stefan-Boltzmann constant), or a fundamental principle (black body radiation, this new albedo-temperature relationship).  No great surprise that some readers have already caught on to some of the issues I wanted to talk about.

One, which I'll continue to defer for now, is the fact Arthur mentioned that what this model works with is the earth's blackbody temperature -- its temperature as seen by how much energy it releases to space -- rather than surface temperature.  Since we all live somewhere towards the surface, surface temperature is the more interesting number.  What the difference between what the model can give us and what we're truly interested in does is to suggest that an important theoretical issue is to develop an understanding of how planetary blackbody temperature relates to surface temperature.  Or (scarier) to see if it does relate in any consistent way.  But heads up that such a discussion will be coming.  Finding these issues, and seeing why they're important, is one of the purposes of the ultra simple models like this.

More issues were brought up by Nick Barnes, who also provides Python code for running your own version (see his first comment for that link).  I hope you've spent some time with either the spreadsheet or Nick's Python (use a 2.7 set-up, per Nick's comment on Tuesday) or do so now, as you read this post, and some more as you decide whether and how it makes sense.  The spreadsheet is in OpenOffice format (.ods) but I've opened that with MS Excel previously.  If you can't, please let me know.

Now, in saying 'issues', I don't mean that there's any terrible comment being made.  Rather, it is the truth that even very simple models like this one have some subtleties that you should explore before drawing your conclusions about nature.  I'll take up the more physical side of interpretation next, but first let's take a look at some of the technical issues.

20 March 2012

Return of the simplest climate model

The simplest climate model balances the energy leaving the earth to space with the energy coming in from the sun.  If the climate is not changing, these two will be the equal.  As long as climate is not changing rapidly, a modifier we can make quantitative, they'll be very nearly equal.  It turns out that even for fairly rapid climate changes, by standards of geological history, the earth is very close to that balance.

I'm actually going to take a different approach this time around.  Key to deciding how much solar energy comes in to the earth (more precisely, the climate system) is knowing the albedo -- what fraction of incoming energy gets bounced right back out.  That makes the model unsatisfactory to me on a theoretical basis.  We have to know the earth's albedo to compute its blackbody temperature (the temperature which provides that balance).  The problem with that is that the albedo itself is a climate term.  The state of the climate -- how many clouds we have, how large the sea ice pack is, how large the continental ice sheets and deserts are, how green the forests are -- determines the albedo.  Knowing either the blackbody temperature or the albedo is a climate observation.  Given one, we can compute the other from that simple model.  And, which is a good point, we can compare our computed temperature with the observed.

Is it possible to remove or weaken that restriction on the albedo?  And if so, can we learn anything about the climate system?  Yes, and yes.

I'll do something that would be quite improper if I were to claim that it was exactly true, but which will turn out to be extremely educational.  Namely, I will make up a relationship between albedo and earth's blackbody temperature. 

20 July 2011

Making your own sea ice estimates

The Sea Ice Outlook does accept estimates from outside the professional community.  Maybe not everybody involved is thrilled by this, but I do think it's a good idea from my distant vantage.  And Jim Overland, one of the people behind the SIO, is strongly in favor of it.  (I had a chance to talk with him about the outlook and other ice matters a few weeks ago.)

In the most recent report, there are 3 submissions from 'outsiders' -- Chris Randles (you've seen him comment here as crandles) and Larry Hamilton, both at Neven's Arctic Sea Ice Blog, and one from Wattsupwiththat.

Watts' entry was a poll of readers.  While perfectly legitimate as an entry, it's also perfectly useless scientifically.  One goal of science is to gain understanding of the system in order to spread the knowledge around.  Polling can't be spread.

Much more interesting are Chris's and Larry's methods.  Both are obviously methods of great brilliance, as they currently have the same estimate as I do from my statistical method -- 4.4 million km^2 for this September.  Beyond that, you can read their method descriptions in the Sea Ice Outlook report and start constructing your own method by not making the mistake they and I have made.  Whatever those turn out to be.  Larry Hamilton's write ups (one for ice extent, one for volume) are:
http://neven1.typepad.com/blog/2011/04/trends-in-arctic-sea-ice-extent.html
http://neven1.typepad.com/blog/2011/04/trends-in-arctic-sea-ice-volume.html

And you can also examine model output from the PIPS replacement model ACNFS, PIOMAS, and CFS as a basis for making your own estimates.   (And please do cite others that you know of.)

All are welcome to post your methods here in addition to (or instead of) at the SIO.

18 July 2011

2011 Sea Ice Outlooks

For 2011, I added a third method of estimation.  Or, rather, I talked with someone who was using a third method and helped refine it some.  Our guesses are 4.4, 4.8, 5.0 million km^2 for September monthly average sea ice extent as computed by NSIDC.

Again, I'll put our estimates in context of some other estimation methods. 
  • Climatology 1979-2000: 7.03 million km^2
  • Climatology 1979-2008: 6.67 million km^2
  • Linear Trend Climatology 1979-2008: 5.31 million km^2
  • Wang, Wu, Grumbine model: 5.0 million km^2
  • Wu, Grumbine, Wang model: 4.8 million km^2
  • Grumbine, Wu, Wang statistical ensemble: 4.4 million km^2
We normally like 30 years for deciding a trend, but 20 years can be enough.  Since it's far from obvious how to decide what is 'climatology' when climate is changing, taking a few different approaches seems a good idea.  I include a climatology which has a (declining) linear trend on the grounds that there clearly is a declining trend to the sea ice extent, so we expect this year to be lower than last year to some degree (on average).

The two climatology means (22 and 30 years) are relatively close to each other, and are far away from anything we've seen in years.  Taking the 30 year trend, from the first 30 years of the satellite record, gives 5.31 million km^2, which is close to a figure seen in recent years (5.36 in 2009), but well above any of our estimates or the 4.9 seen last year.

Below the fold for a few more words about our 3 estimates:

12 March 2010

WUWT trumpets result supporting climate modelling

The recent article at WUWT
NSIDC Reports That Antarctica is Cooling and Sea Ice is Increasing trumpets the observation that Antarctic sea ice is increasing.  This is expected from climate modeling.  Nice to see someone else is picking up on this interesting confirmation of our scientific expectation.

The prediction is old.  In 1992 Manabe and coworkers, in running a changing CO2 experiment, noticed that the Antarctic sea ice cover increased with increasing CO2.  They traced this to increased fresh water on the Antarctic ocean, which derived from increased precipitation -- snow.  They also observed in their model that the Arctic ocean sea ice experienced a marked decline in thickness, and major loss of extent in the summer, but not so large a decrease in the winter.  At the time they wrote, it was still being debated whether there were trends in the Arctic or Antarctic sea ice covers.

The trend in Antarctic ice cover managed to be statistically significant by about 1997, as documented in

D. Cavalieri, P. Gloersen, C. L. Parkinson, J. C. Comiso, H. J. Zwally,
"Observed Hemispheric Asymmetry in Global Sea ice Changes", Science,
278, pp 1104-1106, 1997.  And it was indeed the expected (by Manabe and coworkers) increase.  As well as the expected decrease in the Arctic.

That left the question of the mechanism.  Did Manabe and coworkers identify the correct reason for the sea ice expansion?  Increased snowfall on Antarctic sea ice was documented in 2006 --

Markus, T., and Cavalieri, D. J., "Interannual and regional variability
of Southern Ocean snow on sea ice", Annals of Glaciology, 44, pp 53-57, 2006. (sorry, paywall here).

Since I'm a modeller, I focus on the modelling aspect.  Skeptical science (recently added to blogroll) has a different take about Antarctic sea ice, looking more at atmospheric and ocean temperatures
Watts Up With That's ignorance regarding Antarctic sea ice, with more to come.

12 February 2010

Cloud-temperature feedback

In my three feet of global warming note, I mentioned that two processes in the climate system are a) warmer temperatures -> more moisture in the atmosphere, and b) more moisture -> more severe storms.  A commenter followed up wondering how warming could actually take place, if a) more moisture -> more clouds and  b) more clouds -> cooler temperatures.

A key word there is if.  Although warmer temperatures are observed to lead to more moisture in the atmosphere, it isn't clear that more moisture actually leads to more clouds.  Section 3.4.3 of the IPCC report gives you an overview of the literature on the topic.  Depending on which scientific paper you read, it's more cloud, less cloud, or more over one surface type and less over another.  In other words, an area of significant scientific debate.

It's also a question whether more clouds mean cooler temperatures.  If you're from a cold weather climate, you've experienced that on clear days you get a nice warm daytime temperature, but also a blistering cold nighttime.  Because of those very cold nights, cloudy days can actually average warmer than a sunny day.  The daytime isn't quite as warm, but the night time is far warmer.

Let's take a deeper look in to the relationships between clouds, in particular to look at the feedback on temperature.  You'll notice that the commenter's question is about a feedback -- we start with temperature, and processes occur which ultimately lead to an effect on temperature.  What I'd originally talked about was a straightforward chain.  One thing causes another, causes another.  But no effect on the term or process that started us off.  We'll ultimately get back to the simplest climate model, as it can help shed some light on the question as well.

04 September 2009

One dimensional climate models

Some time back, I described the simplest meaningful climate model, and then gave a brief survey of the 16 climate models.

The next 4 I'll take up are the 4 1 dimensional climate models. These are the models that vary only in longitude, only time, only in latitude, or only in the vertical. It'll be in that order. This turns out to be the order of difficulty, and the order of interest. It isn't until the vertical that we'll get to how exactly it is that the greenhouse effect works.

On the other hand, with the model in latitude we'll see some powerful statements about the fact that energy has to move from the equator towards the pole. Not just the fact, but how much, and how it changes with latitude.

In the model with only time, we can look a little more at things we were thinking towards with the simplest model -- what happens if the solar output varies, or if the earth's albedo does. More is involved, and required, than just that. We'll have to start paying attention to how energy is taken up in the atmosphere, ocean, ice, and land. Not a very large amount of attention -- we can't tell the difference between the poles and the equator, or upper vs. lower atmosphere or ocean. But it's a start.

But for now, let's look at the simplest model in longitude only. As with any of our models, they start with the conservation of energy. The energy coming in is, as before, from the sun. How much energy arrives does not depend on what longitude we're at. Remember, even though the sun rises in the east and sets in the west -- east and west being matters of longitude -- the sun does eventually rise everywhere.

Energy coming in has to be balanced by energy going out. If it weren't, things would be changing over time and there is no time in this model. One part of the energy going out is the solar energy that gets bounced straight out. This fraction is called the albedo. Now albedo is something that can depend on longitude. For instance, land is more reflective than ocean. And along, say, 30 E, the earth is mostly land, while along, say 170 W, it is almost entirely ocean. Clouds can be anywhere. So ... we arrive at one of those unpleasant realities -- we have to get some data.

Normal business. The process arrives at telling us that we need to find averaged albedo over time (say some years) and all latitudes for each longitude. (We don't have to average over elevation because albedo is defined as the energy bounced out -- from whatever level of the atmosphere -- divided by the energy coming in.)

Once we have that, we can compute the temperatures at each longitude that will permit us to balance, with terrestrial radiation out, the incoming energy. These temperatures should be something like the blackbody temperature of the earth we found in the simplest model. But they'll vary some.

The next piece of data we'll need are the observed blackbody temperatures, by longitude. Then we'll compare the simplest model to the observations.

One thing which is possible, and we'll be looking for in our comparison, is that now we've added longitude, a new thing can happen. In the simplest model, the energy coming in had to be balanced, right there, by energy going out. Now that we have longitude, it's possible for energy to shift from one longitude to another. The Gulf Stream and North Atlantic Currents, for instance, move a lot of energy from west to east. If no energy is being transported, on the average, then the temperature for a longitude will be just what we expect. If there's a mismatch, energy has to be getting moved from one longitude to another.

I haven't collected the data yet, so I don't really know how it will turn out. I expect that clouds will cover the albedo differences between land and ocean to a fair extent, so the temperatures we'll compute will be fairly constant. I also expect that heat transport by longitude will be small -- the Gulf Stream's eastward warm current is balanced at least partly by a cool current (relative to local temperatures, that is!) at the equator.

On the other hand, I haven't looked at the data yet, so there is room for surprise. That'll be fun. Means we get to learn more than we expected.

02 September 2009

Models and Modelling

"All models are wrong. Some models are useful." George Box

Box was a modeller, and the sentiment is widely spread among modellers of all kinds. This might be a surprise to many, who imagine that modellers think they're producing gospel. The reality is, we modellers all acknowledge the first statement. We are more interested in the second -- Some models are useful.

But let's back up a bit. What is a model? In figuring out some of this, we'll see how it is that models can be imperfect, but still useful.

There are several sorts of model, is one thing to remember. On fashion runways or covers of magazines, we'll see fashion models. In hobby shops, we can get a model spacecraft or car. We could head more towards science, and find a laboratory model, or a biological model animal, statistical model, a process model, numerical model, and so on.

Common to the models is that they have some limited purpose. A fashion model is to display some fashion to advantage -- making the dress/skirt/make up/... look good. She's not to be considered an attempt to represent all women accurately. The model spacecraft is not intended to reach the moon. But you can learn something about how a spacecraft is constructed by assembling one, and the result will look like the real thing.

In talking about a laboratory model, read that as being a laboratory experiment. You hope that the set up you arrange in the lab is an accurate representation of what you're trying to study. The lab is never exactly the real thing, but if you're trying to study, say, how much a beam flexes when a weight is put in the middle, you might be able to get pretty close. If you want to know the stability of a full-size bridge with full size beams and welds and rivets assembled by real people, it'll be more a challenge -- represent the 1000 meter bridge inside your lab that's only 10 meters long. It won't be exact, but it can be good enough. Historical note for the younger set: Major bridges like the Golden Gate Bridge, Brooklyn Bridge, Tower Bridge, and such, were designed and built based on scale models like this. The Roman Aqueducts designed over 2000 years ago, still stand, and never came near a computer. They were all derived from models, not a single one of which was entirely correct.

In studying diseases, biologists use model animals. They're real animals of course. They're being used a models to study the human disease. Lab rats and such aren't humans. But, after extensive testing was done, it was discovered that the rats for some diseases, and other animals for other diseases, reacted closely enough to how humans did. Not exactly the same. But closely enough that the early experiments and tests of early ideas could be done on the rats rather than on people. The model is wrong, but useful.

Statistical models seem to be the sort that the most people are most familiar with. My note Does CO2 correlate with temperature arrives at a statistical model, for instance -- that for each 100 ppm CO2 rises, temperature rises by 1 K. It's an only marginally useful model, but useful enough to show a connection between the two variables, and an approximate order of magnitude of the size. As I mentioned then, this is not how the climate really is modelled. A good statistical model is the relationship between exercise and heart disease. A statistical model, derived from a long term study of people over decades, showed that the probability of heart disease declined as people did more aerobic exercise. Being statistical, it can't guarantee that if you walk 5 miles a week instead of 0 you'll decrease your heart disease chances by exactly X%. But it does provide strong support that you're better off if you cover 5 miles instead of 0. Digressing a second: Same study was (and is still part of) the support of the 20-25 miles per week running or walking or equivalent (30-40 km/week) suggestion for health. The good news being that while 20 is better than 10, 10 is better than 5, and 5 is way better than 0. (As always, before starting check with your doctor about your particular situation, especially if you're older, have a history of heart problems already, or are seriously overweight). This model is wrong -- it won't tell you how much better, and in some cases your own results might be a worsening. But it's useful -- most people will be better off, many by a large amount, if they exercise.

Process models started as lab experiments, but also are done in numerical models. Either way, the method is to strip out everything in the universe except for exactly and only the thing you want to study. Galileo, in studying the motion of bodies under gravity stripped the system, and slowed it down, by going to the process model of balls rolling down sloping planes. He did not fire arrows, cannon balls, use birds, or bricks, etc.. Simplified to just the ball rolling down the plane. The model was wrong -- it excluded many forces that act on birds, bricks, and all. But it was useful -- it told him something about how gravity worked. Especially, it told him that gravity didn't care about how big the ball was, it accelerated by the same rules. In climate, we might use a process model that included only how radiation travelled up and down through the atmosphere. It would specify everything else -- the winds, clouds, where the sun was, what the temperature of the surface was, and so on. Such process models are used to try to understand, for instance, what is important about clouds -- is it the number of cloud droplets, their size, some combination, ...? As a climate model, it would be wrong. But it's useful to help us design our cloud observing systems.

Numerical models, actually we need to expand this to 'general computational models' as the statistical, process, and even some disease models now, are done as computational models. These general models attempt to model relatively thoroughly (not as a process model) much of what goes on in the system of interest. An important feature being that electronic computers are not essential. The first numerical weather prediction was done by pencil, paper, and sometimes an adding machine -- more than 25 years before the first electronic computer. Bridges, cars, and planes are now also modelled in this way, in addition or instead of scale models. Again, all of them are wrong -- they all leave out things that the real system has, or treat them in ways simpler (easier to compute) than the real thing. But all can be useful -- they let us try 'what if' experiments much faster and cheaper than building scale models. Or, in the case of climate, they make it possible to try out the 'what if' at all. We just don't have any spare planets to run experiments on.

Several sorts of models, but one underlying theme -- all wrong, but they can be useful. In coming weeks, I'll be turning to some highly simplified models for the climate. The first round will be the four 1-dimensional models. Two are not very useful at all, and two will be extremely educational. These are 4 of the 16 climate models.

03 April 2009

How much detail is there really?

I'm thinking about sea surface temperature (SST) these days, but the approach here is one that can be applied to many situations, even ones outside weather and climate. A common, important, and not always easy, questions is -- just how much detail do you need? The more detail, the more expensive it is to make a good product, whether that's an analysis of sea surface temperature, a climate model, or a surface in a video game. Of course, what I'd like is the sea surface temperature every few meters over the entire globe. If that's more than necessary at some time, I could average it down. But ... it would take an awful lot of storage to save temperatures every few meters (my back yard, my neighbor's, my front yard, ...) over the whole globe.

Let's start by looking at an actual high resolution global product, though not every few meters! The SST analysis at http://polar.ncep.noaa.gov/sst/ gives a value every 1/12th of a degree in latitude and longitude, one about every 9 km (6 miles). It has about 9 million values. Let's also suppose that this is fine enough resolution that everything important is represented.

The worst resolution is to use 1 number for the entire globe, the average for all ocean points. To measure how bad this is, I'm going to compute the root mean square error. (Those who know what this is can skip to the next paragraph.) It is often abbreviated rmse. To find it, we go through every ocean point in the grid and find the difference between the value there and the average. Then we multiply this difference by itself (square it -- this avoids the marksmen statistician story*). Then add up these squares for every ocean point. This is a big and not interesting number. One thing that would be more interesting is the average value of the squared error -- the mean square error. So we divide by the number of points that were involved. This also tells us the error variance. Since we think more in terms of temperature and temperature changes than squares of temperature changes, we take the square root of the mean square error -- get the rmse. This is a figure which represents a typical magnitude of how far off we expect to be. We could be either warmer or colder by this much, but this is the magnitude.

* Two statisticians went to a shooting range and each fired at the target. The first missed by 1 meter to the left (-1 meter). The second missed by 1 meter to the right (+1 meter). They then congratulated each other on their fine marksmanship because on average they had hit the bullseye. Their average error was indeed zero. But their rms error was 1 meter.

When I compute the RMSE for using global mean temperature instead of the full resolution grid, I find 12 C. That's ... enormous. The difference between water at 20 C (68 F) and 32 C (90 F) is pretty large! So, clearly, we can't be satisfied with an RMSE of 12 C. But now we have a method for looking at the resolution we need, and a notion of how bad you can get.

Then I made my program average over smaller boxes than the whole globe, say 90 degrees on a side -- London to Chicago, equator to pole -- and found the RMSE comparing those box averages to the original temperatures in the full resolution grid. No surprise that boxes that large were pretty bad. But ... once I got down to boxes 2 degrees on a side (which is something like 200 km, or 120 miles), the RMSE was down to 0.5 degrees.

This is still definitely not zero, but it isn't bad. When a typical satellite used for the job -- such as the AVHRR instrument on NOAA-18 -- is used to make an observation, it has an RMSE (compared to a buoy's thermometer at about the same location at about the same time) of about 0.5 degrees. In other words, with boxes 2 degrees on a side, the average represents what is happening in sea surface temperature about as well as getting a single observation from satellite. We've also managed to reduce our RMS error by about 95% as compared to using only a single number. On the other hand, even though we've captured 95% of what's going on, we only need to use 16,200 numbers -- instead of the 9,331,200 we started with. 95% of the information of the full grid, with only 0.2% as much data.

We've caught 90% of what is happening (reduced the rmse by 90%) when the boxes are 6 degrees on a side (600 km, 360 miles). And it's 99% once we're down to boxes only 0.5 degrees (50 km, 30 miles) on a side (which means only about 3% as many data points are needed to represent the full data set to 99% accuracy).

Now, let's translate this back to some situations we might care about. In trying to construct climatologies of sea surface temperature, we run in to the problem that as we go back in time, there are fewer and fewer data points. On the other hand, if we have 1 observation in each box 6 degrees on a side, we've managed to capture 90% of what is happening in the sea surface temperature. In other words, a much sparser data set than we might imagine could indeed represent an awful lot of what is happening in the ocean. A global grid at 6 degrees resolution has only 1800 points, so we need only 1800 observations to fill it in our simple-minded way.

At 2 degrees resolution, we've captured 95% of what happens in sea surface temperature (at least to this quick little glance -- I only looked at 1 day, as analyzed by 1 center, etc.) So, if we had a good global ocean model at 2 degree resolution, we'd actually be pretty far along in being able to predict sea surface temperatures (model climate, etc.) well. In practice, there are processes that happen in smaller areas than the 2 degree box which can change the whole box's average and we, therefore, want finer resolution than 2 degrees. More about that in a different post.

In thinking about observing systems, if we only 'need' 1 observation every 200 km or so, and we have satellites that can take an observation every 4 km (like the one above) we're all done, right? Unfortunately, no. The problem is, that satellite looks for clouds. If there are clouds -- and cloudy areas can easily stretch for 1000 km -- the satellite can't see the sea surface to tell us what the temperature is down there. So we need other data sources -- ships, buoys, other sorts of satellite (ones that can see through clouds) to fill in even just the 200 km (2 degrees latitude-longitude) boxes each day. Plus we need to observe the detail in the oceans that are involved in those other processes I mentioned. It isn't just for models that they're important -- fishing also cares.

18 February 2009

First successful numerical weather prediction

Wasn't planning on such a gap between posts, but life happens. In the previous note, I talked a little about the first numerical weather prediction. One of the comments (you do read the comments, I hope, lots of good material there!) mentioned an article by Peter Lynch on the first successful numerical weather prediction.

I was of two minds about that article. On the plus side, it is a well-written article about something I'm interested in. On the minus side, I was planning on writing an article much like it myself and now I can't :-( On the plus side, I got to read the article without doing all the work I'd have had to do in writing it myself. In any case, go read it!

The first successful numerical weather prediction was done using the ENIAC computer, and took almost 24 hours to make a 24 hour prediction. I learned numerical weather prediction from George Platzman, who was involved in that effort. When he learned of my interest in history, he gave me copies of his notes from his 1979 lecture, in which he'd re-created the original model. This included, for instance, a lot of work being done to scale all numbers to be a magnitude near 1. The ENIAC did fixed-point arithmetic. If the numbers weren't close to 1, the precision would have rapidly decayed.

One thing I did after programming the model was let it run out farther in to the future than the original 24 hours. The model blew up. A quick check with Platzman showed that this was no surprise. He had (40 years earlier) done the numerical analysis on the boundary conditions and showed that a) they were unstable but b) the instability was 'slow' -- would not affect the 24 hour results. My result confirmed that, though he was surprised that it started to blow up around day 3 and was useless by day 5.

The more refined test, on a model that included the same physical processes but did not include the boundary condition problem, was done by P. D. Thompson, "Uncertainty of initial state as a factor in the predictability of large scale atmospheric flow patterns", Tellus, 9, p275-295, 1957. It appears that he was the first to publish on whether there were intrinsic limits to how far ahead one could predict the weather. Up to about this time, the sentiment had been that if given enough computing power (something much larger than the WPA project Eli mentioned in the previous comments was envisioned by Richardson) and good enough data, then working out the data management (source of Richardson's problems) and numerical representation would suffice to get meaningful answers about weather indefinitely far into the future.

Thompson conducted an experiment on that presumption. Suppose that we start a weather forecast model from two slightly different initial conditions. So slightly different, in fact, that no plausible observing system would be able to tell the difference between them. Would the two forecasts also start and remain too close together for observations to tell the difference? The surprising (at that time) answer was, no. These unobservably small differences would lead to easily observed differences once you were far enough in to the forecast. Worse, 'far enough', wasn't terribly far -- only a week or two.

In 1963, while working on a highly simplified model of convection, Ed Lorenz bought dynamical chaos in to meteorology. Some of his work is described at non-professional level in James Gleick's Chaos: Making a New Science, as are some of the implications. This book was written in 1988, at the peak of the optimism about chaos. Things got messier later. But the history isn't too bad and the descriptions of chaos are helpful.

The key for the moment is that this business of initial states that are quite close to each other giving predictions that are quite different is one of the symptoms of chaos. They're also a symptom of a bad model or programming error, so you have to do some work, as Thompson and Lorenz did, to show that you're dealing with chaos rather than errors.

I started in the previous post with some comments about chaos and climate. We're about ready for those. A couple things to remember are that numerical weather prediction goes back a long way, and that from very early on there have been questions about just how far ahead we could predict weather. What is still open is what any of this -- chaos, limited predictability of weather, difficulty of writing error-free models -- means for climate. More next time.

02 February 2009

Start of Numerical Weather Prediction

I'm going to wind up with chaos and climate, but the route starts with numerical weather prediction. Numerical weather prediction itself starts much farther back than most people realize -- now about 90 years old. And it didn't start with the simplest possible weather prediction model. If you're not up on your history of science and technology, you didn't bat an eyelash at my mention of numerical weather prediction being 90 years old. Electronic computers are only 60-70. 90+ years ago, when the first numerical weather prediction (NWP) was done, 'computer' meant a person who, with pen and paper, slogged through the calculations.

The first NWP was performed by hand, by Lewis Frye Richardson. He did so in between ambulance runs during World War I. The reason he was in an ambulance, rather than the much safer trenches, is that he was a conscientious objector to warfare (Society of Friends (Quaker) by religion). Nevertheless, he did survive the war and completed his numerical prediction. It was finally published in 1922, with it having been essentially completed in 1919.

The model he used was what we now call a primitive equation model. It took the laws of conservation of mass, energy, and momentum in their full complexity and tried to solve them. The first successful numerical weather prediction was not made until about 1948, published in 1950: Charney, J. G, R. Fjortoft, and J. von Neumann, "Numerical Integration of the Barotropic Vorticity Equation", Tellus, 4, 237-254, 1950. It was done on a much simpler equation -- bearing much the same resemblance to the primitive equations as the simplest climate model I've mentioned before does to a full complexity climate model. This model (which Richardson could have done by hand more easily than what he took on) was run on one of the first electronic computers -- ENIAC.

The first model to implement something comparable to what Richardson tackled was not done for another 2 decades after the ENIAC model (the '6 layer PE' model Shuman, F. G., and J. B. Hovermale, An Operational Six Layer Primitive Equation Model", J. Applied Meteorology, 7, 525-547, 1968).

In any case, Richardson's forecast has often been called a glorious failure in the ensuing decades. The failure part being that the forecast was so drastically in error -- predicting a surface pressure change of over 100 mb, when only 6 or so would have been considered large. He did recognize the likely sources of his problem, but doing this kind of computation by hand was too expensive (in time) to do multiple trials to nail down exactly which was the source of his problem and which idea for repair would take care of his problem.

The glorious aspect is his enduring contribution to the field. For starters, he invented numerical weather prediction. Much of what is done today is still dependent on approaches he invented. He also foresaw massively parallel processing, and one of the central problems in that -- making sure that your different processing 'nodes' (people, in his case, computer processors in ours) remained synchronized.

For more on Richardson's forecast, see especially Weather Prediction by Numerical Process, by Lewis F. Richardson. Original publication in 1922, republished in 1965 by Dover Publications. This is the original, full, document. More recent consideration was made by G. W. Platzman, "Richardson's Weather Prediction", Bull. Amer. Meteor. Soc., 60, 302-312, 1968. Platzman includes discussion of the sources of Richardson's problems. There is a later note in BAMS by Platzman giving more considerations and ideas.

02 January 2009

Happy Perihelion

Not quite yet, but as everyone else is wishing happy New Years that seems covered. On the 3rd (usually at least) of January we are closest to the sun. That the calendar year starts near then is coincidence. Due to orbital variations (Milankovitch cycles), our date of closest approach varies through the calendar year. This is the longitude of perihelion.

Back with the simplest climate model posts we looked some at how our distance to the sun could affect the global mean temperature. In honor of our passage, a project to see how much difference our being 0.0167 astronomical units closer to the sun than normal (i.e., we'll be at 0.9833 AU instead of the average 1.0000) would make. At least, would make if the assumptions of the simplest model were all true.

14 September 2008

The 16 Climate Models

The number of climate models, in the sense I'm using, has nothing to do with how many different groups are working on modelling climate. I'm sure the latter figure is much larger than 16. Instead, it is an expansion on my simplest climate model, and can give a sense of what lies down the road for our exploration of climate modelling.

The simplest climate model is the 0 dimensional model. We average over all of latitude, longitude, elevation, and time (or at least enough time). Those are the 4 dimensions we could have studied, or could get our answer in terms of. The 0 dimensional model gives us just a number -- a single temperature to describe everything in the climate system. We could expand, perhaps, to also getting a single wind, humidity, and a few other things. But it's distinctly lacking in terms of telling us everything we'd like to know. It fails to tell us why the surface averages 288 K, instead of the 255 K we see as the blackbody temperature. But it does get the blackbody temperature a start.

There is also only one 4 dimensional model -- where you include all 4 dimensions: latitude, longitude, elevation, and time. These are the full climate models, also called general circulation models (GCMs), atmosphere-ocean general circulation models (AOGCMs -- the original GCMs only let the atmosphere circulate), and a few other things. These are the most complex of the models.

But there are 14 more climate models possible: 4 one dimensional, 6 two dimensional, and 4 three dimensional.

In one dimension, we have the four which let 1 dimension vary, only:
  • time
  • elevation
  • latitude
  • longitude

Something quite close to the simplest model can be used for the time-only climate model. We would then let the earth-sun distance vary through the year, solar constant vary with the solar cycle, and albedo ... well, that would be a bit of a problem. As we've still averaged over all latitudes and longitudes, however, this model wouldn't tell us about why high latitudes are colder than low latitudes, or why land on the eastern side of oceans is warmer than land on the western side, or ... a lot. Still, it would take us another step of complexity down the road to understanding the climate system on global scale. This sort of model isn't used much professionally, but it can be a help

In elevation only, we'd (we hope) be able to look in to why the temperatures in the atmosphere do what they do -- falling as you rise through the troposphere and mesosphere, even or rising in the stratosphere. This class of models is known as the Radiative-Convective models (RCM). Namely, they include radiation and convection. The most famous early model of this sort is by Weatherald and Manabe, (1967?). We'll be coming back here.

In latitude only, we'll start being able to see why the poles are colder than the equator. Budyko and Sellers, separately but both in 1969, developed models like this. They're called energy balance models (EBM). They start with our simplest climate model, but applied to latitude belts on the earth. First you pretend that no energy enters or leaves the latitude belt except through the top of the atmosphere. Same thing as we said for the simplest model, except we applied it to the whole earth. You then compute the latitude belt's temperature, and discover that the tropics would be much warmer than they are, and the polar regions would be much colder. We're not surprised that we get the wrong answer here, but the degree of error then tells us by how much and where this 'no latitudinal energy transport' approximation is worst. You can then add the physics of 'heat flows from hot to cold' and get to work on how the climate in your model changes due to this fact.

The 4th one dimensional model, I've never seen anyone use -- a model in longitude only. This dimension is much quieter than the other two spatial dimensions. In the vertical, global average temperatures vary by something like 100 C in something like 10 km. 10 C/km; we'll get to exactly how much, where, and why, later. In latitude, temperatures vary from 30-40 C in low latitudes to -40 to -80 C in high latitudes (poles), so rounding again, about 100 C, but now across 10,000 km. About 0.01 C/km. In longitude, after we average over all year and all latitudes, ... there isn't much variation. As an eyeball matter, I'd be surprised if it were more than 10 C. (Project: Compute it. Let me know your result and sources. I may eventually do it myself.) This would be not more than 10 C, but still across 10,000 km or so, so something like 0.001 C/km at most (average absolute magnitude).

So our 4 models can be sequenced in terms of how much variation they get involved with, and, not coincidentally, it's something like the order of frequency I've seen the models in the literature:
  • Elevation -- Radiative-Convective Models (RCM) -- 10 C/km, 100+ C range
  • Latitude -- Energy Balance Models (EBM) -- 0.01 C/km, about 100 C range
  • Time -- (not common enough to have a name I know of) -- a few C range, seasonally
  • Longitude -- (never used that I know of) -- 0.001 C/km or less, a few C range

The 6 two-dimensional models are:
  • time-elevation (an expanded Radiative-Convective Model)
  • time-latitude (an expanded Energy Balance Model)
  • time-longitude (I've never seen done as a model, but Hovmo"ller diagrams do this in data analysis)
and then to ignore time, and take
  • elevation-latitude (a cross between Radiative-Convective and Energy Balance)
  • elevation-longitude (I've never seen as a model, but it's not unheard of for data analysis)
  • latitude-longitude (I've never seen as a model, but common for data analysis)
The three that don't involve longitude are (or at least were) relatively common for models.

In 3 dimensional modelling, we are back down to 4 models, as for 1 dimensional. This time, though, it's a matter of what we leave out:
  • time (keep latitude, longitude, elevation; not common for models)
  • longitude (keep time, latitude, elevation -> the straight combination of RCM and EBM; most common of the 3D models)
  • latitude (keep time, longitude, elevation)
  • elevation (keep time, latitude, longitude)

And then we have kitchen sink, er, 4 dimensional, modelling.

A question I'll take up later is why we would run a simpler model (1d instead of 2d, 3d instead of 4d) if we could run the more complex model. Part of the answer will be that there's more than one way to be complex.

01 September 2008

Summary1 of Simplest Climate Model

First, a much-delayed suggestion to go look at Atmoz's calculation of the effect of the earth being an oblate spheroid rather than a perfect sphere. More about that in a moment.

The simplest model discussion so far occupies a few posts:
In making the correction for the earth being an oblate spheroid rather than a perfect sphere, Atmoz found the 4 in the original formula (simplest model) should be changed to 4.00449, at least when we're at the equinoxes. As the earth's orientation changes, it will present somewhat different areas to the sun. Imagine a pancake, as an example of an extremely oblate spheroid. Put a pencil through it (the short direction) and consider that the rotation axis of your very oblate planet. Have a friend hold it up and tilt it some from the vertical. As you walk around your friend, you'll see the pancake edge on (equinoxes) and then more of the top or bottom as you get to the solstices. The amount of tilt will affect how much your view varies. The more tilt, the more variation. The earth is tilted about 23.5 degrees from the sun.

Atmoz found about a 0.07 degree C difference for the earth's temperature for oblate (and at equinox) vs. perfect sphere. Probably something about that size too for the solstices too, though we need the computation to be sure.

Here I've used an albedo of 0.30 and solar constant of 1367 W/m^2. Atmoz preferred 0.29 and 1366, respectively. Thanks to our looking into the sensitivity of the model in the analysis note, we know that this amounts to only about a 1 K difference in computing the earth's temperature. That suggests a few things. One is, the surface temperature averaging 288 K is unlikely to be explainable by modest changes from the values we used. Another is that it'd be a good idea to chase down some good sources on what values should be used, exactly. Or that at least we'll want to find out what the levels of uncertainty are about these observable quantities.

11 August 2008

Analyzing the simplest climate model

Before we try to solve the problem of why the temperature around us averages about 15 C (288 K) instead of the -18 C (255 K) we found in the simplest model, let's look some more at the model. It depends on 3 things -- the sun's energy input to the earth, the albedo of the earth, and the average distance between the earth and sun. How much does it depend on those things? By the end, we'll also have another site to ignore for its unreliability.

We know that the sun's output can vary by about 1 Watt per square meter during a solar cycle. So try computing the temperature with 1368 instead of 1367. Try again with 1366. How much difference does that make? I get about 0.05 K (0.09 F). That's a pretty small number. We'd be hard-pressed to get a thermometer to record it.

How about the albedo? I find about a 1 K change (0.9) for a 0.01 change in albedo. Such a change in albedo (or to increase it by this much) is plausible for the earth, though 0.10 would be a wild value, not expected by anybody I know of. Quick sanity check ... why is the albedo so much more important than solar term? Albedo multiplies the solar constant. The natural variation is 1 Watt per square meter. The 0.01 change in albedo means a 13.67 Watt per square meter change in energy entering the climate system, so we expect it to be much larger. (project: why is it 19 times more important rather than just 13.67?)

The mean distance from the earth to the sun does change -- on a long enough time scale. Changes in the earth's orbital eccentricity (how circular vs. how oval-shaped) can give changes in average distance of something like 0.001 AU. This translates to about 0.18 K (0.32 F) variations in earth's temperature to space. (These are Milankovitch variations in eccentricity, with the fastest time scale of change being 100,000 years; some are over 2 million years).

If we take those sizes of temperature change and divide by how fast they occur, we get a sense of which is most important for thinking about climate change on our time scale of interest. The sun's output changes along a solar cycle of about 11 years. The earth's albedo changes with the seasonal cycle, so 1 year. And the eccentricity is 100,000 years. Looking at degrees per year, we then have:
  1. Albedo 1 degree per year
  2. Solar cycle 0.005 degrees per year
  3. Eccentricity 0.000002 degrees per year
So, if we're thinking about weather and climate over the next few years to centuries, the obvious candidate to be paying attention to is the albedo. Eccentricity changes too little and too slowly, and the solar cycle returns to its start before the century is up (net of zero change), and is much smaller than the albedo effect can be on a few year scale (albedo doesn't go in the same direction for a long time, but just how long and how much needs some thinking).

Variations in solar output and the earth's orbit are not part of the climate system itself, and the orbit can be predicted to very high accuracy for a very long time into the future. In terms of understanding the climate system, both the solar and orbit factors are good -- given these non-climate terms, we can compute a climate. If we know the albedo.

But what is albedo? It's the bouncing of energy from the sun back to space. Now what does that bouncing? Well, everything in the climate system -- clouds, gas molecules, ocean surface, trees, grass, desert, dirt, glaciers, snow cover, ice packs, ... The gas molecule term depends little on the climate, and, if I remember correctly, would bounce about 15% of the solar input even if the earth's surface were a perfect solar absorber (perfectly black). But it isn't; even the ocean, which is about the darkest part of the earth's surface, reflects at least 6% of the sun's energy (that reaches it), and that figure increases as the sun gets low in the sky.

If none of these things changed their albedo as the climate got colder or warmer, we'd only have an annoyance -- can't give a climate figure without looking at the system. But the extent of deserts, ice sheets, sea ice, ... does change depending on climate temperatures. That 'about 0.30' albedo is correct for recent times. It may not be correct in an ice age earth or an even warming than present earth. Consequently, while we can use this model to understand some points about the climate system, we can't use it to predict full climate responses. We're not surprised, since we're much warmer at the surface than the blackbody temperature. But this is an additional reason we're going to want a more complex model down the road.

On the other hand, it does help us understand the system -- we know now that albedo is very important, and how much it and solar input could be expected, on a simple basis, to affect climate.

We also, it turns out, have a tool for identifying unreliable sources. I was surprised to see this be the case, but Steve Milloy at junkscience(dot-com)/Greenhouse assumes that if there were no clouds, the earth's albedo would be zero. Even knowing nothing about the details of albedo, you know this has to be wrong. If the earth's albedo, aside from clouds, were zero, you couldn't see the earth except for the clouds. As this image reminds us, you can indeed see the earth from space. His writing where he makes the error says:
We should note that devoid of atmosphere Earth would actually be a less-cold -1 °C (272 K) because the first calculation strangely includes 31% reflection of solar radiation by clouds
He also seems to be calculating the solar constant rather than taking an observed value, and using odd values for the his calculation.

Project: what would be better values for each figure, and how would using them affect his results?

07 August 2008

Building the Simplest Climate Model

Where did the simplest model come from? Nice that I showed a model that gives realistic answers, but even better to know how it works!

The model is built on one of the great conservation laws of science -- conservation of energy. If you track all the ways that energy enters your 'system', and all the ways that it leaves, you can know quite a lot about it even without knowing very much about what's going on inside. That word 'system' may not mean what you're thinking. What I mean here is that we draw an imaginary box around, in this case, the earth, and see what passes through the box.

We have, in general, three ways to get energy through the box. We can carry some material from one side to the other (advection or convection). But the earth doesn't gain or lose material from space, so can't gain or lose energy this way. Another way is to conduct heat across the boundary. A frying pan does this in making the handle hot even though the flame is a good distance away. But with a vacuum on the other side of our box, there's nothing to conduct to. The third way is as radiation. Everything emits some radiation. The hotter is is the more it emits. A traditional thermos tries to minimize all three -- the inside is glass, a poor conductor, the glass is almost totally surrounded by a vacuum to cut down conduction even further, it is sealed, to prevent convection, and the inner wall of the thermos is reflective, to prevent the wall from gaining or losing heat by radiation to your drink.

In looking at what can cross the boundary of the earth system we have only two things -- radiation from the sun, and radiation from the earth. We all know that many things can happen inside the box: storms, building and melting ice sheets, forest growth and decay, and so on. But they're all inside. For our simplest model of the temperature of the earth we don't need to know about those, just income versus outgo. (Well, more to it than this, but hang on for now.)

The sun's radiation all comes in to the box, passing through a disk whose area is pi*r^2, where r is the radius of the earth and pi is the usual 3.14159... Same as the sun and moon look like disks to us, we look like a disk to the sun. Some of that solar energy gets bounced right back out. The fraction of the incoming solar energy that gets bounced out is called the albedo. For the earth, it is about 0.30 averaged over the whole planet, through the whole year. Particular surfaces can be much higher (snow can be 0.8) or much lower (oceans can be 0.06). But since we're only concerned with what passes through the box, we don't need to worry about those details yet.

The earth also emits radiation, as does everything that's not at absolute zero. For an ideal black body, that emission is proportional to s*T^4. This is the Stefan-Boltzmann law, and s is the Stefan Boltzmann constant, equal to 5.67e-8 Watts per square meter per K^4. Every square meter of the earth radiates like this. Since the earth is (very nearly) a sphere, the total area is 4 * pi * r^2. Again, r is the radius of the earth.





Conservation laws are written in terms of a balance of income and outgo. If the earth is in energy balance, then the following equation is exact. If it isn't, we'll have to look at how far out we are.
Income = pi * r^2 * S

Outgo =
pi * r^2 * S * a (albedo reflecting energy immediately away from the earth)
+ 4 * pi * r^2 * s * T^4

For the conservation law being Income = Outgo, we get
pi * r^2 * S = pi * r^2 * S * a + 4 * pi * r^2 * s * T^4

We notice two things rapidly. First, pi * r^2 is in every term. We can divide the equation by that and simplify. Second, the solar term is on both sides. We can subtract the albedo term from both sides to get all the solar-related terms on one side, and the earth on the other. So now we have:

S*(1-a) = 4*s*T^4

If we solve for T, we're back to the equation I gave in the original note

It's remarkable that the size of the earth doesn't show up here. Actually, it does -- that 4 is the remaining part. It's 4 because the entire area of the (spherical) earth emits energy to space, while the sun only contributes energy through a circular disk, and the area of the sphere is 4 times larger than the area of that disk.

This leads to a point that I see commonly missed. When solar observers talk about how much the solar output changes, they're referring to the S -- seen by the disk of the earth. During a solar cycle, it varies by about 1 Watt per square meter. In looking at climate, though, we think in terms of the spherical earth we're standing on, rather than the disk in space a satellite is using. When climate people talk about Watts per square meter, we're talking about 4 times as many square meters as solar observers. To make the two comparable, climatologists often divide the equation by 4, meaning that when a solar observer says 1 Watt per square meter, climate folks will treat it as 0.25. Not because we don't think the sun's important, but because the 0.25 gives a description that we can compare to earthly climate processes we observe all over the sphere.

On Monday, there'll be a third post in this set -- analyzing this model. In the mean time, a project for the more mathematically skilled out there: How is this model affected by using a proper oblate spheroid for the earth? Is it? And, for everyone, try out the spreadsheet version and see how it behaves as you change the parameters.

Ah, I should note that the S above isn't exactly the S in the original. Here it's the solar constant divided by mean earth-sun distance (in AU), while I left the two separate in the original. As tamino showed, the two are awfully close to each other since the mean earth-sun distance (over a year) doesn't change much even as the orbit varies on tens of thousand year time scales.

A different and more important matter if you're not used to this is that the temperatures will come out in Kelvin -- the scientific absolute temperature scale. Celsius is used, but when we are concerned about energy, it's best to use Kelvin (K). Fahrenheit is probably never used in doing science (even if someone did, it never gets published that way). Kelvin is Celsius plus 273, so water freezes at about 273 K, boils at about 373 K. (Or Celsius is Kelvin minus 273.) The earth's black body temperature is about 255 K, or -18 C.