If you don't see an index on the left, click here.

Guide to Aurora Sentry Data

This guide is an unofficial collection of notes on the use of Aurora Sentry data. In no way should this ever be considered a substitute for official information from the organizations who provide the data. Please check the web sites of the providers for official information.

This document is a work in progress. Updates will be made at irregular intervals.

 

Definition of Terms
   Poleward? Equatorward? North? South? Arrgh!!

Oval Estimates
   CANOPUS Auroral Oval
   STD Visible Auroral Oval
   NOAA POES Statistical Auroral Activty (North)
   NOAA POES Statistical Auroral Activity (South)

Earth Imagers
   POLAR VIS Image
   POLAR Ultraviolet Imager
   WIC image

Magnetometers
   North America: Boulder, Colorado
   North America: Fredericksburg, Virginia
   North America: Newport, Washington
   North America: College, Alaska

   Europe: Wingst, Germany
   Europe: York, UK

   Pacific region: Learmonth, Australia
   Pacific region: Canberra, Australia

Solar wind and Dst Index
   SEC Solar Wind Dials
   UC Berkeley Dst Index
   Costello Predicted Kp Index
   ACE MAG and SWEPAM
   SRI Dst Index and Solar Wind
   SoHO Proton Monitor

Solar Activty, etc.
   GOES Xray Flux
   GOES Satellite Environment
   SoHO EIT 195 Å
   Yokoh SXT Image

Definition of Terms

Poleward and Equatorward
When discussing aurora, and dealing with northern and southern hemispheres (users of this site come from all over the globe) the terms north and south can be confusing. What we usually want to know is whether some location is closer to the [north or south] pole than another, or whether some location is closer to the equator than another. Therefore we use the terms poleward and equatorward. Poleward means "closer to the pole" (north in the northern hemisphere, south in the southern hemisphere). Equatorward means "closer to the equator" (just the opposite of poleward).

 

Oval Estimates
Oval Estimates attempt to provide an overall visual indication of the extent of the auroral oval(s) plotted on a map in near real time. Aurora Sentry displays this page by default.

CANOPUS Auroral Oval
Data from the CANOPUS magnetometer chain (Canada) is used to calculate the poleward and equatorward boundaries of the northern auroral oval, with the result plotted on a map of the northern hemisphere. Color variation corresponds to auroral intensity. This is the only oval estimate derived from ground based instruments. It has been found to be a valuable guide to the relative intensity and equatorward boundary of the radio aurora. A large scale intensification or equatorward expansion of the oval should be a warning to get to the radio or go outside and check the sky. With experience many users (especially those in North America) find this plot very useful in estimating local conditions.

STD Visible Auroral Oval
Based on data from the NOAA POES satellite, this plot is intended as a guide to where the aurora should be visible. This tends to lag real time to some extent. The color changes from green through brown and eventually to red as the aurora intensifies. Aurora is most likely to be visible within the shaded areas near the equatorward boundary of the auroral region.

NOAA POES Statistical Auroral Activity (North)
A statistical estimate of the position of the northern auroral oval based on data from the NOAA POES satellite. Intensity of auroral activity is rated on a scal of 1 to 10. Generally very high values (9 or 10) would indicate aurora in the northern continental U.S. Tends to lag real time somewhat.

NOAA POES Statistical Auroral Activity (South)
A statistical estimate of the position of the southern auroral oval based on data from the NOAA POES satellite. Intensity of auroral activity is rated on a scal of 1 to 10. Tends to lag real time somewhat.

 

Earth Imagers
Earth Imagers are satellite "views" of Earth which show the aurora. These are not visible images as would be seen by the human eye or a camera, but what is seen by various imaging equipment on the spacecraft. The update interval on these varies and the images tend to lag behind real time, but can provide valuable information. Pay particular attention to the date and time on these images, as they are not always current.

POLAR VIS Image


POLAR Ultraviolet Imager


WIC image

 

Magnetometers


North America: Boulder, Colorado


North America: Fredericksburg, Virginia


North America: Newport, Washington


North America: College, Alaska



Europe: Wingst, Germany


Europe: York, UK



Pacific region: Learmonth, Australia


Pacific region: Canberra, Australia

 

Solar Wind and Dst Index
Our sun is hot and stormy place. It continuously emits a stream of fast moving inoized gas (plasma) called the solar wind which flows out through the solar system. This solar wind also has magnetic fields contained within it. Events on the sun control the "strength" of the solar wind. Coronal holes cause the wind to escape the sun at a higher than normal velocity. Coronal mass ejections often accompany strong flares (and other solar events), and these can cause drastic disruptions in the solar wind. The solar wind is always interacting with Earth's magnetic field, and these interactions change during times of disturbed conditions, causing what is known as a geomagnetic storm on Earth.

The data in this section is based on measurements by satellites located in line between the sun and Earth (but much closer to us than to the sun). From here we can get a near real time indication of what is happening in the solar wind as it approaches Earth. Because these satellites are located some distance from our planet, we see the conditions in that part of the solar wind that is 30 to 60 minutes away from Earth. This can be very important, giving a warning when conditions on Earth are about to change. Some Aurora Sentry users watch this page almost exclusively during storm times in order to have a feel for what is about to happen with the aurora.

Several properties of the solar wind are measured. Among the most important for our purposes are the speed of the solar wind (in kilometers per second), its ion density, and most important the magnitude and orientation of magnetic fields within the solar wind. "Southward oriented" magnetic fields in the solar wind interact with Earth's magnetic field much more than neutral or northward oriented fields.

Some caution is in order when using data based on measurements from the ACE satellite. During some storm times, protons hurled into space from powerful solar flares may interfere with the instruments' ability to provide meaningful data. If the ACE-based data seems to indicate "all quiet" while other data is indicating storm conditions, this is probably the cause.

SEC Solar Wind Dials
Using data from the ACE spacecraft, these dials show the most important measured parameters: magnetic Bz component (strength of the magnetic field in the north-south direction), speed, and dynamic pressure. Note the color coding on the dials; as the pointers move more toward the red portion of the scales, the chances of geomagnetic storming (and aurora) increase. Most important of all here is the Bz, which really needs to be southward (-) to produce storm conditions on Earth. The dials are very convenient, but show only an instantaneous "sample" of solar wind condtions. Current trends are best observed using some of the other data in this section.

UC Berkeley Dst Index
Computed from ACE data, this is a convenient dial that gives the current near real time Dst estimate. Yellow indicates mild storm, red is strong storm conditions. Dst is an index that monitors the worldwide magnetic storm level. Negative values of Dst indicate a storm in progress (only negative values shown on this dial). The actual Dst index is computed from many magnetograms from ground based instruments around the world. The data provided here is an estimate of what that Dst index will be based on measurements of the solar wind.

Costello Predicted Kp Index
Based on ACE data, this is a computation of the predicted Kp index. The blue line shows actual observed Kp. This source is very useful for seeing recent conditions at a glance, with an estimate of short-term future trends as well.

ACE MAG and SWEPAM
This is the "raw" data from ACE. It is very good for observing both short term fluctuations and long term trends. The white Bt trace in the top panel is the total field strength (total intensity) of magnetic fields in the solar wind, while the red Bz trace is the magnetic field intensity in the very important north-south direction. Bt (and often Bz) increase during storm times. Sustained southward Bz will be necessary to produce geomagnetic storming and aurora for all but the most poleward locations. Density and speed are also important parameters. In particular, a sudden increase of 50 units or more in speed probably indicates arrival of a shock front ahead of a disturbance. It is important to note the main phase of the disturbance is often several hours behind the shock front.

SRI Dst Index and Solar Wind
This is another useful plot based on ACE data which color codes the very important Bz parameter: green when there is little or no chance of significant storming; yellow for slight or moderate chance; red for strong chance of storming. From the raw data, current Dst estimate and storm conditions are computed.

SoHO Proton Monitor
This is the one item in this section that is not based on data from ACE. Instead this one uses solar wind measurements from the SoHO spacecraft, which is not subject to "blackouts" from proton contamination. The top two traces (solar wind speed and density) show very clearly when a disturbance has arrived.

 

Solar Activity, etc.
Solar activity is what drives the solar wind, and disturbances in the solar wind drive geomagnetic storms. It is therefore a good idea to keep an eye on potential storm-inducing events on the sun. Such events would include coronal mass ejectioons or CMEs (which often occur in conjunction with major solar flares) and coronal holes. It takes 1 to 4 days for a disturbance to transit from sun to Earth in the solar wind.

GOES Xray Flux
From the GOES satellites, this is a near real time measurement of solar radiation in the form of X-rays. Solar flares are readily apparent as spikes in the plot, but it is important to remember that not all flares are associated with a CME. Solar flares are classified according to their peak intensity and fall into "bins" of C, M, or X class. "Major flares" are those reaching M5 or higher. Caution must be used here, but typically a flare associated with a large CME will have a very rapid rise, slow decay signature. CMEs can and do occur when there is no flare and little or no X-ray signature is apparent. In addition, many large CMEs which will show up in X-ray data are not "aimed" at Earth and will have little or no impact on conditions here. Still, this is a very useful chart that shows when conditions are getting stormy on the sun.

Examples of impulsive flares (usually not associated with a large CME) and a long duration flare. The long duration flares with this type X-ray signature are often accompanied by CMEs capable of producing geomagnetic storms.
Typical X-ray signature of a long duration flare associated with a CME. A severe geomagnetic storm arrived only one day after this powerful X class event.


GOES Satellite Environment
Several useful measurements of the near-Eath space environment are made by the GOES satellites. The top panel (Proton flux) is a measurement of energetic protons, usally associated with poweful solar flares. Proton levels here will be elevated (generally above the dashed line) at times when the ACE sensors (see Solar Wind section of this document) are experiencing "proton contamination". The third panel (Hp) is from the onboard magnetometer and wild fluctuations occur during geomagnetic storms. The bottom panel shows the Kp index color coded green (quiet or unsettled), yellow (active) and red (storm).
GOES satellite environment plot during storm time. Notice the proton event (top panel). ACE sensors were adversely affected by this event. A severe geomagnetic storm peaked late on July 15.


SoHO EIT 195 Å
A usfeul image of the sun from the Extreme Ultraviolet Imager on the SoHO spacecraft. At this particular wavelength (195 angstroms), coronal holes appear as dark (black) areas. Coronal holes near the sun's polar regions (top and bottom of the image) have little impact on conditions at Earth, but holes that traverse the center of the image near the solar equator can cause the solar wind speed to increase, sometimes dramatically. Coronal holes are long duration features which will be observed to move across the image as the sun rotates on its axis, appearing in the east (left) and rotating toward the west (right). As a coronal hole passes the center of the solar disc, the solar wind streaming out through it is aimed toward Earth; the maximum affect will be observed 2 to 4 days after the hole passes the center of the image, due to transit time from sun to Earth. Solar active regions (typically associated with groups of sunspots) appear as bright areas.
EIT 195 Å image showing a coronal hole approaching the central meridian. Three to four days later solar wind speed increased to around 600 km/s and the geomagnetic field was at active to minor storm levels


Yokoh SXT Image
This image from the Yokoh satellite shows solar radiation in the form of X-rays. The dark areas are "bright" in X-rays, usually associated with active sunspot groups. If major flares occur while the larger, more intensely active regions traverse the center of the solar disc (facing Earth), the chance of a disturbance reaching Earth increases.