# Optical Phenomena of Ducts

## Introduction to ducts

What's a duct? It's a layer of air whose temperature gradient is sufficiently steep to make the curvature of horizontal rays greater than that of the layer, so that some rays get bent back to lower levels. The cause of ducting is a thermal inversion with a lapse rate more negative than about −0.11 K/m; see the bending page for numerical details.

Here's the temperature profile for the rather modest duct I use to illustrate ray paths in the superior and mock mirages:

Basically, it's just a two-degree (Celsius) thermal inversion between 50 and 60 meters height, superimposed on the Standard Atmosphere. But, as explained elsewhere, the corners have been rounded off to allow for the real-world effects of heat transfer.

## Duct optics

Optical ducts produce a surprisingly complex set of phenomena. What you see depends on where you are: above, below, or in the duct. The observer's location is particularly critical near the bottom of the duct. That's why this page is called “Optical Phenomena of Ducts” rather than “Optical Phenomena in Ducts”.

Here, we have simulations of the effects of ducts on sunsets. For ducts and mirages, see the other duct page, which shows ray-traces in ducts.

### Discontinuous images

First, the duct produces discontinuities in the images. That's because a ray that's horizontal just above the top of the duct always remains above the duct; but a ray that's horizontal just below the top of the duct gets bent downward in both directions. This second ray meets the bottom of the thermal inversion at some considerable angle, and propagates into atmospheric layers well below the inversion.

In this lower layer, the ray curvature is less than the Earth's curvature, so the surface of the Earth gradually bends away from the ray. If the duct is far enough above the surface of the Earth, these latter rays eventually become parallel to the surface, and then ascend into the duct again — whence they can be bent back down another time, and so on, ad infinitum. Such rays are trapped in the duct forever (assuming the thermal structure that created the duct goes on forever); see the mirage page for a ray-trace.

So an observer within the duct sees only trapped rays in a zone of sky that is symmetric about the astronomical horizon. This zone of trapped rays is Wegener's “blank strip”. (Indeed, it was Wegener who first pointed out these discontinuities.)

But even an observer above the duct sees discontinuous images: a ray that's just tangent to the top of the duct is horizontal there, so all rays higher in the observer's sky avoid the duct. But rays even a little lower must enter the duct, where they receive a large angular deviation. The refraction of all objects seen through the duct is much greater than that of objects seen just above it; so again, the images are discontinuous at the top of the duct.

Observers below the duct see a continuous, but highly distorted, image of the sky near the astronomical horizon.

### Infinite refraction

There's another startling feature of refraction in ducts. At the edge of the thermal inversion, there's always a height where the ray curvature is exactly equal to the Earth's curvature. A horizontal ray at the height must circle the Earth at constant height “forever” (i.e., until it's extinguished by atmospheric extinction.)

But, once again, you don't have to be exactly at this height to see the phenomenon. Any observer above the duct can look just above it and see rays that (in principle) can approach the critical level and circle the Earth once, twice, … before escaping back to space. The closer you look to the top of the duct, the bigger the refraction becomes — without limit!

In the real world, extinction prevents us from seeing rays that have had refractions more than a few degrees. But even the rays we can see produce some remarkable effects: images of the entire Sun compressed to a thin line at the top of the duct, for example. Of course, these images occur at the edges of the image discontinuities, producing some very startling effects.

[These circulating rays were studied in a remarkable paper by Kummer in 1860. If you read German, it's a fascinating work. He shows that circulating rays can produce an infinite number of images of everything! The whole sky, and the whole surface of the Earth, are re-imaged an infinite number of times, in his model.]

### … and it's all modified by dispersion

As if these remarkable phenomena weren't enough, remember that the refractive index of air depends on wavelength. That means all the phenomena described above are different in different colors of light. Combining the effects of dispersion with the monochromatic optics of ducts produces the astonishing sub-duct green flashes.

Sorry to have this sudden change in appearance; we need to turn down the lights in the following sections, so that details in the darker parts of the sunset images can be seen. A white background just drowns them out.

## Examples

To illustrate the phenomena of ducted sunsets, here are some examples. Each image has a short commentary to point out its significant features.

Because different phenomena are seen from different heights, I've made different groups of simulations for the same atmospheric structure, as seen from heights:

But, rather than jumping around, you'll see what's going on best by viewing these cases in order. These links are provided so you can go back and review them, if you want another look at one or two.

Bear in mind that the effective exposure of our simulated sunset camera is increased automatically as the Sun sinks into the haze; the relative brightnesses within each image are correct, but the brightness changes from one image to the next mean nothing, because the “exposure” is adjusted to show as much dynamic range as possible.

It's simplest to begin with the observer well above the duct, and then move the eye down, because things get more complex near the bottom of the duct.

## Sunset seen from 100 meters height

This sunset has an aerosol scale height of 1 km, and an optical depth above the observer of 0.035. These values correspond to clear conditions, and make the increased extinction below the duct obvious, without obscuring things too much.

In the image at the right, the true altitude of the Sun's center is −25′ of arc. The low Sun appears flattened, as usual; atmospheric extinction dims and reddens the lower limb. Even so, the color of the Sun is orangish, not deep red: the air is unusually clear.

The only indication of anything unusual is a slight change in brightness of the sky, about halfway between the lower limb and the apparent horizon. This is the discontinuous change in haze optical depth at the duct.

At the the left is the second image in this sequence. The Sun's center is now 40′ below the astronomical horizon.

Part of the disk is now below the false horizon at the duct. However, a mock mirage of the lower limb is beginning to appear in the zone between the duct and the apparent horizon. Note that this dim image shows an inverted image of the lower limb in its upper half, and an erect (but vertically stretched) image of the same little piece of the lower limb in its lower half. The sides of this little image are vertical at a folding zone where there is infinite vertical magnification.

Under average conditions, the extinction might obliterate that mock-mirage image completely. Then the false horizon at the duct would be interpreted as the true apparent horizon — but it would have a dip several minutes of arc less than normal.

In the image at the right, the Sun's center is 50′ below the astronomical horizon. This depression corresponds to the standard tables for the nominal time of sunset.

About half the disk is now below the duct. The mock mirage of the lower limb has become a large blob that nearly fills the space between the duct and the apparent horizon. You can see that the inverted image of the lower limb has become very compressed just below the duct. The vertical magnification changes rapidly from great expansion (in the middle of the sub-duct zone) to great compression (just below the duct.)

Also, the infinite refraction at the duct makes a dark line in the sky, which is now more visible because the increasing exposure is making the sky features more obvious.

When the Sun's center is 56′ below the astronomical horizon, the part below the duct appears nearly rectangular. That's because the center of the Sun is at the zone of maximum vertical magnification, and the inverted image of the lower limb (just beneath the duct) is strongly compressed.

If you look closely, you can see that the part of the solar image just above the duct shows thin “spikes” or “whiskers” that extend the full width of the Sun, beyond the cap of disk that remains above the duct. These are caused by the infinite refraction just above the duct.

At a depression of 56′, the part below the duct is beginning to shrink. The “waist” in this image is at the fold line, where the erect (lower) and inverted (upper) images of the lower limb join.

The part of the solar image just above the duct is now reduced to a thin line that's barely visible in this image. If the aerosol extinction were greater, or if the aerosol were more concentrated below the duct, this bright line would be more conspicuous.

Here's a series of 3 images, showing how the waist below the duct breaks. At a depression of 71′, the waist has narrowed down. At a depression of 72′, the waist has broken, but the two parts are still visible. At −73′, the part below the break has vanished below the apparent horizon, leaving just a thin red strip below the duct. This strip is the inverted (i.e., mock-miraged) image of the disappearing upper limb. (The image that was above the duct has now disappeared, extinguished by the ever-increasing extinction as it approaches the duct from above.)

In principle, a faint green flash might be observed at the horizon under extremely clear conditions; you can see a faint green rim on the disappearing erect image of the upper limb in the second of these three images. In practice, the large extinction beneath the duct makes the green rim very faint. So in practice, these flashes aren't observable.

You can see how this is going to end. The inverted image of the upper limb fades away just below the duct, as its erect image above the duct vanished, due to the increasing extinction that accompanies the approach of refraction to infinity.

The clearer the air, the longer this process can be observed. This image has a solar depression of 85′; if the air were clearer, it might be followed to well over 90′. However, the image is very thin, because the observer is so far above the duct. A lower eye level prolongs this appearance, by increasing the angular thickness of the thin line.

## Sunset seen from 65 meters height

Here's the same atmospheric model, but seen from 65 meters height. The haze model is also very similar, with 1-km scale height and 0.035 optical depth above the observer — but now that's at 65 meters instead of 100.

Remember that the thermal inversion responsible for the duct extends from 50 to 60 m above sea level in this model. So our observer is now just 5 m above its top. This makes the duct-top features considerably more visible than they were from 100 m.

This first image is for a solar depression of 20′. It's similar to the first image in the previous sequence, but the duct appears higher above the apparent horizon, because the observer is closer to it.

At a solar depression of 34′, the mock mirage of the lower limb appears in the sub-duct sky. Again, it's dim and red, because of the large extinction.

At a solar depression of 50′, the mock mirage of the lower limb below the duct has become nearly rectangular.

The image above the duct shows the “spikes” better than at 100m, because we are closer to the top of the duct. (A photograph of a sunset like this is shown on Les Cowley's website.) This image resembles the “tin hat” worn by the AEF in WW I, as pointed out by Willard J. Fisher, in his description of Type B sunsets (which are also produced by strong thermal inversions below eye level). Fisher's Type B sunsets were usually observed from just a few meters above a surface-based inversion, so they resemble this image with the part below the duct cut off.

At −55′, the image above the duct has shrunk to a thin, bright line. The image below the duct is starting to become narrower, as the upper half of the Sun descends through the mock-mirage zone of sky.

These four images, in 1′ steps from −65′ to −68′, show the breaking of the neck between the erect and inverted parts of the mock mirage. The interval between successive images is 4 or 5 seconds of time at low latitudes.

The erect image of the upper limb at the apparent horizon takes longer to set than it did at 100m, because the observer's lower position makes the duct appear higher above the apparent horizon here.

As before, the sunset ends in a thin line that fades away at the duct, as this image at −80′ shows.

And once again, there's no green flash for this observer.

An animation of a similar sunset (the same atmosphere, but seen from 70 m height instead of 65 m) is available.

## Sunset seen from 50 meters height

Now, let's move down into the duct itself. You might think the middle of the duct would be the middle of the inversion layer; but, as the duct is caused by the bending the inversion produces, its effects are strongest at the bottom of the inversion — in this case, about 50 meters. So let's take that height as the place to see the maximum effects of ducting. (We continue to use the same atmospheric model as before.)

As Wegener showed, an observer in the duct sees a “blank strip” at the astronomical horizon. In this strip are the trapped rays; as they can't get out of the duct, none of them can lead back to the Sun (or any other astronomical object). So the sky seems to be split apart at the astronomical horizon: everything that was close to the duct in the sky (as seen from above the duct) gets shoved aside. That means there's strong image compression near the blank strip, both above it and below it.

Here's the Sun when its center is geometrically 15′ below the astronomical horizon. Notice how much flatter it is on the bottom than in similar views for an observer above the duct: that's the image compression at work.

Also, see how the discontinuity in sky brightness at the duct has been replaced by a gap in the bright sky: the blank strip. Distant terrestrial objects in the duct can be seen miraged in this zone; we don't have any in the simulation, however.

But that dark strip in the sky becomes really interesting when the Sun crosses it, as in the next images.

Here on the right is the Sun when its center is geometrically 30′ below the astronomical horizon. Its lower limb is completely squashed against the top of the blank strip. In addition, a mirage of the lower limb, heavily reddened, is appearing below the strip.

This mirage is a curious mixture of mock mirage and Wegener's Nachspiegelung. Notice that the image compression applies to it, on the upper (inverted-image) side, where the strip is squeezing it together.

As in the previous series, the image below the duct is much dimmer than the part above the duct, because of the greatly increased airmass in the line of sight.

At −40′, the Sun looks like a pot with a lid, separated by the blank strip. The lower limb is now below the apparent horizon; and the Sun's center is compressed beyond visibility on top of the strip. The lip of the “pot” is of course part of the inverted image of the lower limb.

At −50′, the lid of the pot is flattening out and about to disappear. The sides of the pot are now beginning to shrink together at the fold line between erect and inverted images of the upper half of the Sun.

This image shows, more plainly than the previous ones, the red edges of the blank strip. The reason is dispersion: the strip is wider at short wavelengths, because the refractive index is bigger there. So there's no blue or green light at the edges of the blank strip in red light; the only thing seen at these edges is long-wavelength images of the Sun.

At −61′, the lid of the pot has vanished, and the sides have collapsed to a point. Nothing remains visible above the blank strip. The crossover, just below the strip, marks the fold line: the part of the Sun above it is an inverted and highly distorted image of the upper limb, just as the larger part below the crossing point is an erect and highly distorted image of the upper limb. The green fringes that flank the crossing point are distorted images of the green rim — but, once again, are too dim to produce a visible green flash.

At −65′, the erect image is about to disappear at the horizon, while the inverted image is fading fast as a thin red line just below the blank strip. At −66′ (right image), this process is nearly complete; a tiny wisp of green rim is just vanishing at the apparent horizon.

This sunset can be seen as a simple animated cartoon. It gives a good impression of the relative speed at which the features develop, but of course the intensities are all wrong, so the extinction features that were pointed out above are not represented correctly.

## Sunset seen from 46 meters height

The observer remains within the duct, but below the inversion layer, for several more meters. Here's the view from 46 m, just above the bottom of the duct, and about 4 m below the inversion.

With the Sun 15′ below the astronomical horizon, its image is entirely above the blank strip, which is now much narrower. The flattening of the lower limb is, as expected from the previous case, considerable.

At −30′, the Sun is split into two unequal images. The upper one, above the blank strip, is a distorted but entirely erect image; the lower limb is strongly flattened by the strip. The lower image is a doubled partial image of the lower limb; the lower part of it is erect, and the upper part, just below the blank strip, is miraged (inverted) by the Nachspiegelung. (See the mirage page for a ray-trace of the Nachspiegelung.)

At −50′, the nominal depression at sunset, we still have several minutes of arc of solar image above the blank strip, which itself extends several minutes of arc above the astronomical horizon (its centerline). This shows how much refraction the duct has added to the “normal” value.

Note that the red edges of the strip are more pronounced in this case. This is an example of the increase in dispersion effects at the bottoms of ducts.

At −60′, the erect and inverted images of the upper limb below the blank strip have separated; but there is still some of the limb left above it. This produces an interesting triple image of the upper limb.

However, the subsequent development is not very interesting. The thin stripes flanking the blank strip become narrower and fade away, while the piece of upper limb at the apparent horizon simply sets and disappears, without producing a green flash.

## Sunset seen from 45 meters height

Now let's move down just one more meter, to 45 m height. This is enough to put the observer just below the duct, so it closes up the blank strip.

You wouldn't think a shift in position of a single meter would make a major difference in the sunset's appearance, but it does. Let's have a look:

This first image isn't very startling. The Sun (at −15′) is strongly flattened on the bottom, but that's what you'd expect in this situation.

As we are now below the duct, it's no longer marked by a line in the sky, because we no longer have a line of sight that's tangent to its surface. So this is a pretty unexciting picture, apart from the rather large flattening of the Sun's lower limb.

At −30′, the closure of the blank strip has made the image mapping smooth and continuous; so the Nachspiegelung of the lower limb now joins smoothly with its erect image immediately above. Nothing very startling there, either.

However, there is a harbinger of things to come. Notice how much wider the red rim on the lower part of the image is than the green rim on top: the dispersion effects are large in the Nachspiegelung zone.

Notice, too, that a vertical line placed across the edge of the lower bulge can intersect the same point on the lower limb three times: once in the inverted part of the image, and twice in the erect parts, above and below it. This will shortly have interesting consequences.

At −40′ we have the pot-with-a-lid appearance again, but this time the lid is firmly joined to the pot.

At −50′ the sides are beginning to shrink in, as the middle of the Sun lies below the Nachspiegelung zone.

However, you can now begin to see what will happen: when the top of the Sun reaches the region of triple images, it can pinch off and produce a green flash. And the part of that green flash in the zone of enhanced dispersion effects can be larger than usual.

Sure enough, a blob pinches off at the top of the Sun at −59′, and turns green at −59.9′. And what was a wide red rim on the lower limb has now become a wide green rim on the upper.

The last two images here show the evolution of that green flash at −60′ and −60.1′. But it still remains visible until −60.3′. This is the sub-duct flash. (An even larger example is shown here .)

Those images are for the same atmosphere model we've been using, with a haze optical depth of 0.035 above the observer, and a haze scale height of a kilometer. The flash looks a lot better if we trap most of the haze below the inversion, though. Let's cut the scale height to 50 meters, and reduce the opacity above the observer to 0.004:

That's the same sub-duct flash as in the image directly above it; the Sun is at −60′. The only difference is in the haze model — here I've tweaked it to suppress the red disk at the horizon and reduce the brightness of the red aureole, so that it doesn't dilute the flash as much as before.

After the flash shrinks to nothing, it's an ordinary sunset. The remaining disk sets at the apparent horizon by −65′.

On the other hand, this sub-duct flash is already a lot nicer than a mock-mirage flash, even though this was a fairly weak duct of only 2° (here's a mock-mirage flash, with a similar aerosol model, for comparison):

Notice how puny the mock-mirage flash (right) looks, compared to the sub-duct flash (above).

An important difference between these two flashes is their horizontal width, which is an indication of how long they last. (The duration depends on how thick the miraged green rim is, which determines how long it takes to set or disappear; but that also determines how wide the flash is from left to right, because the Sun's radius is fixed.) Sub-duct flashes can last a lot longer than the ordinary green-rim flashes due to inferior mirages and mock mirages.

## Sunset seen from 40 meters height

Now let's move down a few more meters, to 40 m. At this height, the effects of the duct are much weaker. I'll just show a couple of images for solar altitudes that were most sensitive to the duct, above. (We're back to our usual haze model once again.)

The images above for solar depressions of 30′ were all marked by strong mock-mirage and/or Nachspiegelung effects. Here's the view from 40 m for that depression.

There's certainly some distortion. And, if you recall the appearance at this depression from higher elevations, where there was a miraged image below the duct, you can see a hint of that effect here. But there's no miraging.

At −40′, there's still a hint of the pot-with-a-lid effect. But it's just a hint, here.

At −50′, the Sun looks a bit square-shouldered.

You can see this isn't leading to anything interesting. The disk is a bit mis-shapen, but it's not spectacular. There's no hint of a green flash in the works; the Sun just sets and that's it.

This last case illustrates how overwhelmingly important the layers near eye level are on the shape of the sunset, and the occurrence of green flashes. There can be all sorts of interesting thermal structure in the atmosphere; but if it's more than a few meters (or a fews tens of meters, at most) above you, its effects are quite small.

A technical discussion of why the layers near and below eye level are so much more important than the upper atmosphere is in my 2004 paper in the Astronomical Journal.