IlluminationXXVI_425

Illumination XXVI, Jokulsarlon, Iceland, 2012

French microbiologist Louis Pasteur famously remarked, “Chance favors the prepared.” Just showing up doesn’t guarantee success. You can stack the deck in your favor by being prepared. To be prepared you have to find answers to a lot of questions – or at the very least know what questions to ask … like where to go, when to go, how long to stay, what to bring, how to use what you bring, what you hope to accomplish, what your priorities are, and what you bring to the situation that is unique, for starters.

To get this image (and others like it), I had to do a lot of preparation. I thoroughly understood the subject; following Yogi Bhajan’s advice ““If you want to learn something, read. If you want to understand something, write. If you want to master something, teach.” I had done all three. I was in the right place; Iceland is on the auroral oval. I was there at the right time: as Iceland is just south of the arctic circle, skies are dark enough for a long enough period of time at only certain times of the year. I brought the right equipment; a sturdy tripod with a good mount and a fast lens were essential, plus there was new game changing camera technology that generated less noise at higher ISOs, which would open up new possibilities. I knew how to use the equipment; using your camera in the dark and focusing on a star doesn’t become fluid without some practice. I performed relevant tests to find out how much time it took before stars trailed and how high I could dial my camera’s sensitivity up before without getting objectionable levels of noise. I learned from my failures; after careful examination of images from the previous week I found out how shallow the depth of field or focus was at very fast apertures and that certain lenses produced unacceptable artifacts. I took stock of my community’s previous accomplishments; I looked at a lot of images of auroras, identifying what made some more successful than others. I made some time for self-reflection; I noted what was likely to make my images more authentic and what would make them more likely to stand out from others’ images, either on their own or through their relation to my other work, and I prioritized what I wanted to accomplish. All of this preparation contributed to my being able to work quickly and make the most of each passing moment in a focused way that was most likely to generate results that were relevant to satisfying my goals.

It was so easy to make dramatic images that night and there were so many other photographers making images around me that the bar was raised, which called me to succeed not just on others’ terms but more importantly on my own terms and not just once but multiple times.

Some preparation is specific to a task and/or a moment. A great deal of preparation is more general and cumulative. Often, one builds on the other. Author Malcolm Gladwell suggests that mastery comes when we put in 10,000 hours. Even if you haven’t put in the 10,000 hours to achieve general mastery you can still master the moment; and if you have put in the time, you’ll be able to master many more moments. I’ve often been asked, “How long does it take you to make an image?” I answer, “Anywhere from 15 minutes to 6 months – but the real answer is 47 years and counting.”

Questions

How many kinds of preparation do you need to do – physical, mental, emotional, communal? Why?

What kind of preparation do you need to do the most/least of? Why?

At what point do you get diminishing returns from continued preparation?

Can you be overprepared?

When does preparation become avoidance?

Find out more about this image here.

View more related images here.

Read more The Stories Behind The Images here.

How Auroras Work

November 12, 2012 | Leave a Comment |

The science behind the breathtakingly beautiful phenomenon of  the nocturnal light shows called auroras is fascinating.

The layers of the sun’s atmosphere (photosphere, chromosphere, corona) become increasingly cooler, moving away from its core at15 million degrees Celsius to its surface at 6,000 degrees Celsius. Sunspots, visibly dark areas within the sun, or areas of significantly lower temperature, 4000 degrees Celsius, occur continuously, ebbing and peaking in frequency in 11 year cycles. High sunspot counts correlate with high levels of solar activity. Unlike the bright loops of energy that can be seen on the sun’s surface as particles flow along lines within the sun’s magnetosphere, the darker areas or coronal holes exist where magnetic lines have only one anchor point in the sun’s magnetosphere, allowing plasma to escape.

This plasma carries part of the sun’s magnetic field with it; the interplanetary magnetic field or IMF. The density of the solar wind decreases with distance but its sphere of influence, the heliosphere, reaches past our solar system’s outer planets. The sun’s rotation causes this field to radiate in a spiral structure.

The speed of the solar wind averages 450 km/s but often varies significantly from 300 km/s to 1000 km/s. Large variances in the solar wind’s velocity, density, and magnetic can cause significant terrestrial disturbances.

The solar wind constantly distorts the earth’s magnetic field (caused by the rotating metallic fluids of its core) compressing it on the light side, into a half sphere, and elongating it on the dark side, in a tube, similar to the shape of a comet’s tail. As the supersonic solar wind approaches the obstacle of the earth’s magnetic field a shock front is formed; as the solar wind is directed around the earth, smaller magnetic waves occur between the earth and the sun slowing and changing the course of the streaming plasma.

Surrounding the axis of the magnetic field, offset 11 degrees from the geophysical axis, are weaker areas that give energy rich solar particles little resistance. The charged solar particles that do make it into the upper atmosphere (ionosphere) excite electrons causing them to jump to higher orbits temporarily before they return to their original orbits by giving off auroral radiation and producing visible light in the process.

Auroras (borealis in the north and australis in the south) are produced by the solar wind, fast-moving charged particles that escape the sun’s gravity, exciting gases in the earth’s upper atmosphere.

The color of auroral emissions is determined by the gases excited, primarily oxygen and nitrogen. Altitude also influences color; red is found above 200 km, yellow and green between 180 – 110 km, and blue and violet below that. These altitudes vary between dayside and nightside aurora; at night blue and green altitudes drop increasing in intensity, while red rises decreasing intensity.

Auroras appear most consistently, almost continuously, and intensely in an oval band that rings the magnetic poles; in the north 67 degrees magnetic latitude at magnetic noon and 76 degrees magnetic latitude at magnetic midnight. Additionally a thinner weaker band of increased occurrence bisects this oval along a straight line between the sun and the earth.

Auroras occur by night and by day. The difference between night and day auroras is the number of particles (greater in the day), the amount of energy the particles carry (less by day), and the dominant color (green by night, red by day). Dayside aurora only occur inside the auroral oval at high polar latitudes and are only visible when it is dark during the day.

Auroras are extremely dynamic. Their zone of maximum occurrence can change by several hundred kilometers in minutes. And they can vary in orders of magnitude within seconds.

It’s small wonder that these fantastic colored lights that dance in mesmerizing patterns filling the heavens above have held a never-ending fascination for those who are lucky enough to witness them, whether first or second hand. They’re divine.

Learn more about night photography in my digital photography workshops.

Find out about my Iceland Auroras workshop here.


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