A Traveler s Guide to the Aurora
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- Audrey Bell
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1 A Traveler s Guide to the Aurora A description of the aurora, how to predict its occurrence and how best to view it by Professor Charles Deehr Auroral Forecaster The Geophysical Institute University of Alaska Fairbanks
2 from the Solar System A Traveler s s Guide to the Aurora
3 The Biggest Show on Earth A Traveler s s Guide to the Aurora
4 Any planet with an atmosphere has aurorae.. The planet s magnetic field makes it special. The Earth s magnetic field acts as a generator, sending current along the field lines towards the atmosphere around the poles. Magnetic Fields of Sun & Earth
5 The aurora is an unrivaled natural wonder. On Earth, it forms a circle around the poles. The Biggest Show on Earth
6 Venus no magnetic field The airglow is created by electromagnetic radiation from the sun. The aurora is concentrated particle bombardment of the atmosphere guided by remnant magnetic fields. A Traveler s s Guide to the Aurora
7 The aurora is concentrated particle bombardment of the atmosphere guided by remnant magnetic fields Mars no magnetic field
8 Jupiter largest magnetic field The giant planets have huge magnetic fields. This concentrates the particle bombardment to the poles and restricts direct access from solar wind. Most of the aurora is internally generated A Traveler s s Guide to the Aurora
9 Jupiter Jupiter aurorae is produced by energetic particles from its planets and from its magnetic field radiation belts. There may be some produced by the solar wind. A Traveler s s Guide to the Aurora
10 Saturn medium magnetic field Saturn s aurorae are similar to Jupiter s.
11 Saturn Saturn s s aurora are more active than Jupiter s. This is evidence that the solar wind more directly influences the aurora.
12 Closer to home, a view from the Shuttle From 400 km above the Earth, we can see that it is suspended in the atmosphere about 100 km above the surface. A Traveler s s Guide to the Aurora
13 Incomparable Light in the Sky A Traveler s s Guide to the Aurora
14 An Array of Colors A Traveler s s Guide to the Aurora
15 Color from the Earth s Atmosphere The colors of the aurora come from the nitrogen and oxygen molecules and atoms in the atmosphere. A Traveler s s Guide to the Aurora
16 Classify According to Color Type a - crimson upper border Type b magenta lower border Type c green arc Type d red overall Type e magenta and green lower border Type f blue or purple A Traveler s s Guide to the Aurora
17 Classify According to Color Type b Magenta Lower Border
18 Classify According to Color Type c Normal Green, Gray
19 Classify According to Color Type d Great Red Aurora
20 Classify According to Color Type e Magenta Moving Ahead Of Green
21 Classify According to Color Type f Blue or Purple Sunlit Aurora
22 Classify According to Color Type f - Blue or Purple Sunlit Aurora A Traveler s s Guide to the Aurora
23 Color Due to Local Ionosphere A Traveler s s Guide to the Aurora
24 Forms Differ With Local Time A Traveler s s Guide to the Aurora
25 Forms Differ With Local Time A Traveler s s Guide to the Aurora
26 Forms Differ With Local Time A Traveler s s Guide to the Aurora
27 Forms Differ With Local Time A Traveler s s Guide to the Aurora
28 Auroral Forecast Begins at the Sun A Traveler s s Guide to the Aurora
29 Auroral Forecast Begins at the Sun A Traveler s s Guide to the Aurora
30 Auroral Forecast Begins at the Sun Invention of the telescope led to sunspot counting and close solar observation. Cycles of 11 years, 100 years and?. Aurora correlates with sunspots. Historical aurora sketchy measure of solar activity. A Traveler s s Guide to the Aurora
31 The Aurora in History Before 1700, aurorae were viewed as a sign of something in the sky. Ezekiel in Bible Babylonian tablets Chinese astrologers Greeks & Romans Beowulf Charles Morton
32 11 year solar cycle A Traveler s s Guide to the Aurora
33 Two Types of Solar Activity Type 1: Fast streams from coronal holes exist for several solar rotations Type 2: Eruptions from solar events produce shock and exist for few hours
34 Coronal Holes Type 1: Fast streams from coronal holes exist for several solar rotations. They enhance auroral activity each time they sweep by (28 days).
35 Fast Streams in the Solar Wind A A model of the solar wind developed at the Geophysical Institute shows the part of the solar wind that is otherwise invisible. The solar wind is like a garden sprinkler. The fast streams from the coronal holes crowd the field lines.
36 Effect of Coronal Holes on Aurora Auroral activity repeats with 27 day solar rotation Auroral Forecast up to months in advance
37 Type 2: Solar Events Type 1: Fast streams from coronal holes exist for several solar rotations Type 2: Eruptions from solar events produce shock and exist for few hours
38 Coronal Mass Ejection (CME) Type 2: Eruptions from solar events produce shock and exist for few hours. A coronograph on a satellite shows the solar wind near the sun. An explosion sends material, electrons and protons out into space. A Traveler s s Guide to the Aurora
39 Coronal Mass Ejection (CME) Type 2: Eruptions from solar events produce shock and exist for few hours. When the material is a halo around the Sun, it is heading toward Earth. Its arrival affects the satellite camera.
40 Disturbance in the Solar Wind Type 2: Eruptions from solar events produce shock and exist for few hours. The shock and some of the material takes days to reach Earth.
41 The The Venusian Venusian Connection Connection Oxygen and carbon ions observed in the wind from Venus Evidence for transport of microbes from Venus A Traveler s Guide to the Aurora
42 Resulting Aurora The magnetic field of the solar wind links up with the magnetic field of the Earth and the solar wind power is transferred to the Earth s s magnetic field where it drives electrical currents into the atmosphere creating the aurora.
43 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp varies from Levels of Auroral Activity
44 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp varies from Levels of Auroral Activity
45 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp varies from Levels of Auroral Activity
46 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp varies from Levels of Auroral Activity
47 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp varies from Levels of Auroral Activity
48 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp varies from Levels of Auroral Activity
49 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp varies from Levels of Auroral Activity
50 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp varies from Levels of Auroral Activity
51 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp varies from Levels of Auroral Activity
52 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp varies from Levels of Auroral Activity
53 The more power injected into the Earth s s magnetic field the greater the extent of the aurora. The measure of this activity is the planetary magnetic disturbance index, Kp. Kp = 3 is most common Levels of Auroral Activity
54 Aurora Australis Captain Cook first recorded sighting the aurora australis while sailing the Southern Ocean on the way to New Zealand in February and March of 1773.
55 The Southern Hemisphere The sun rises in the east and sets in the west in both hemispheres, but travels from left to right in the north and right to left in the south. Auroral features follow the same directions in both hemispheres, but look different to the observer.
56 The sun rises in the east and sets in the west in both hemispheres, but travels from left to right in the north and right to left in the south. Auroral features follow the same directions in both hemispheres, but look different to the observer. Conjugate Mirror Images
57 The Conjugate Flights Because the magnetic field lines have aurora at both ends, we designed an experiment to see if the aurorae at both ends were similar in type, brightness and occurrence. A Traveler s s Guide to the Aurora
58 The Conjugate Flights In the 1960s there were two airplanes maintained by LANL in readiness for nuclear test monitoring. These planes were used in a number of auroral studies, one of which was the conjugate flights.
59 The Conjugate Flights Narrow field cameras were located in the rabbit windows and recorded amazing conjugate details.
60 The Alaskan Aurora is Brighter The magnetic field is weaker at the same altitude above Alaska than above New Zealand.
61 The Aurora Australis Where would you go to see the aurora in the Southern hemisphere? This is the maximum extent of the aurora. This occurs about once every 10 years. A Traveler s s Guide to the Aurora
62 A more realistic appraisal is shown here. This is average activity. The number of people under the aurora australis is less than the population of Fairbanks. The Aurora Australis
63 The equivalent activity in the northern hemisphere is on the edge of very populated areas. The Aurora Borealis
64 The brightness and occurrence frequency is greatest over Alaska and Eastern Russia. The skies are clear more often over Alaska and Eastern Russia. Two Reasons to go West
65 Two Reasons to go West The brightness and occurrence frequency is greatest over Alaska and Eastern Russia. The skies are clear more often over Alaska and Eastern Russia. Auroral zone Cloudiness Index
66 Alaska and the Yukon are Therefore Best Conclusion: relative to the rest of the world, the aurora is brighter, more frequent and accessible and in clearer skies in Alaska and the Yukon.
67 There are few roads to the aurora. Secondary roads and some air access is availble in Canada, but east of Manitoba, the weather deteriorates. Auroral zone A Traveler s s Guide to the Aurora
68 Away from city lights On a summit or open country With a clear view of the horizon, especially to North and West Prepare to stay up late sometimes 3 4 am. Watch the 1 hour auroral forecast. Watch the weather forecast. The Best View
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