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Coronary Mass Ejections control 1-year Short Term Climate Changes
definition:
Coronary Mass Ejection is subset of Coronal Mass Ejections,
directly targeting the Earth
subjects to study:
Aurora Borealis (Northern Lights)
Weather.gov > Sioux Falls, SD > Aurora Borealis (Northern Lights)
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The Aurora Borealis (commonly referred to as the Northern Lights) are the result of interactions between the Sun and Earth\'s outer atmosphere. The Aurora Australis is the southern hemisphere counterpart to the Aurora Borealis.
What Causes the Aurora? The Sun emits electrically-charged particles called ions, which correspondingly move away from the Sun in a stream of plasma (ionized gas) known as the solar wind. As the plasma comes in contact with the Earth\'s magnetic field, the ions will be agitated into moving around the Earth. Some of the ions become trapped and will consequently interact with the Earth\'s ionosphere (an average of 60-80 miles above the surface), causing the ions to glow. This is the same principal as how a neon sign lights up. As electrons pass through the neon tubing, they glow, thus producing the light in a neon sign.
The Aurora are constantly changing and moving in streams of light or curtains, because the process of how the Sun\'s ionized gas interacts with the Earth\'s magnetic field is very dynamic. Although harmless to life on Earth, the Aurora can cause power disruptions in satellite communications and in radio/TV broadcasts.
Aurora Displays: The northern latitudes (or southern latitudes in the southern hemisphere) see the greatest occurrence of the Aurora. In the northern hemisphere, there is a 50% or greater chance of seeing Aurora roughly between the latitudes of 55 to 80 degrees north. This means in general that in these latitudes, the Aurora should occur on at least half of the nights throughout the year. However, this also varies. Aurora displays usually increase during times of the solar maximum. They also usually show a greater frequency during the winter months, where the nights are longer and the skies generally void of haze. Although most common in the northern latitudes, the Aurora have been occasionally seen south of 35 degrees north latitude which encompasses the far southern United States. Displays this far south can occur when a large coronal mass ejection from the Sun creates a huge geomagnetic storm in the Earth\'s outer atmosphere. This occurred on the night of November 5th and 6th, 2001 where amazing Aurora displays were seen as far south as Texas, Arizona and San Diego, CA
https://www.weather.gov/fsd/aurora
Coronal Mass Ejections
Coronal Mass Ejections (CMEs) are large expulsions of plasma and magnetic field from the Sunâs corona. They can eject billions of tons of coronal material and carry an embedded magnetic field (frozen in flux) that is stronger than the background solar wind interplanetary magnetic field (IMF) strength. CMEs travel outward from the Sun at speeds ranging from slower than 250 kilometers per second (km/s) to as fast as near 3000 km/s. The fastest Earth-directed CMEs can reach our planet in as little as 15-18 hours. Slower CMEs can take several days to arrive. They expand in size as they propagate away from the Sun and larger CMEs can reach a size comprising nearly a quarter of the space between Earth and the Sun by the time it reaches our planet.
The more explosive CMEs generally begin when highly twisted magnetic field structures (flux ropes) contained in the Sunâs lower corona become too stressed and realign into a less tense configuration â a process called magnetic reconnection. This can result in the sudden release of electromagnetic energy in the form of a solar flare; which typically accompanies the explosive acceleration of plasma away from the Sun â the CME. These types of CMEs usually take place from areas of the Sun with localized fields of strong and stressed magnetic flux; such as active regions associated with sunspot groups. CMEs can also occur from locations where relatively cool and denser plasma is trapped and suspended by magnetic flux extending up to the inner corona - filaments and prominences. When these flux ropes reconfigure, the denser filament or prominence can collapse back to the solar surface and be quietly reabsorbed, or a CME may result. CMEs travelling faster than the background solar wind speed can generate a shock wave. These shock waves can accelerate charged particles ahead of them â causing increased radiation storm potential or intensity.
Important CME parameters used in analysis are size, speed, and direction. These properties are inferred from orbital satellitesâ coronagraph imagery by SWPC forecasters to determine any Earth-impact likelihood. The NASA Solar and Heliospheric Observatory (SOHO) carries a coronagraph â known as the Large Angle and Spectrometric Coronagraph (LASCO). This instrument has two ranges for optical imaging of the Sunâs corona: C2 (covers distance range of 1.5 to 6 solar radii) and C3 (range of 3 to 32 solar radii). The LASCO instrument is currently the primary means used by forecasters to analyze and categorize CMEs; however another coronagraph is on the NASA STEREO-A spacecraft as an additional source.
Imminent CME arrival is first observed by the Deep Space Climate Observatory (DSCOVR) satellite, located at the L1 orbital area. Sudden increases in density, total interplanetary magnetic field (IMF) strength, and solar wind speed at the DSCOVR spacecraft indicate arrival of the CME-associated interplanetary shock ahead of the magnetic cloud. This can often provide 15 to 60 minutes advanced warning of shock arrival at Earth â and any possible sudden impulse or sudden storm commencement; as registered by Earth-based magnetometers.
Important aspects of an arriving CME and its likelihood for causing more intense geomagnetic storming include the strength and direction of the IMF beginning with shock arrival, followed by arrival and passage of the plasma cloud and frozen-in-flux magnetic field. More intense levels of geomagnetic storming are favored when the CME enhanced IMF becomes more pronounced and prolonged in a south-directed orientation. Some CMEs show predominantly one direction of the magnetic field during its passage, while most exhibit changing field directions as the CME passes over Earth. Generally, CMEs that impact Earthâs magnetosphere will at some point have an IMF orientation that favors generation of geomagnetic storming. Geomagnetic storms are classified using a five-level NOAA Space Weather Scale. SWPC forecasters discuss analysis and geomagnetic storm potential of CMEs in the forecast discussion and predict levels of geomagnetic storming in the 3-day forecast.
*Images courtesy of NASA and the SOHO and STEREO missions
https://www.swpc.noaa.gov/phenomena/coronal-mass-ejections
3. Tracking coronary mass ejections
Coronal Mass Ejections - NASA/Marshall Solar Physics
https://solarscience.msfc.nasa.gov/CMEs.shtml
Coronal mass ejections (or CMEs) are huge bubbles of gas threaded with magnetic field lines that are ejected from the Sun over the course of several hours. Although the Sun\'s corona has been observed during total eclipses of â¦
AUTOMATIC DETECTION AND TRACKING OF CORONAL MASS â¦
https://www.osti.gov/biblio/22037009-automatic...
20.06.2012 · Studying coronal mass ejections (CMEs) in coronagraph data can be challenging due to their diffuse structure and transient nature, and user-specific biases may be introduced through visual inspection of the images. The large amount of data available from the Solar and Heliospheric Observatory (SOHO), Solar TErrestrial RElations Observatory ...
New Tool Could Track Space Weather 24 Hours Before Reaching â¦
https://www.nasa.gov/feature/goddard/new-tool...
Jun 9, 2015 New Tool Could Track Space Weather 24 Hours Before Reaching Earth A giant cloud of solar particles, called a coronal mass ejection, explodes off the sun on Jan. 7, 2014, as seen in the light halo to the lower right in this image captured by ESA/NASA\'s Solar and Heliospheric Observatory.
Coronal mass ejection - Wikipedia
https://en.wikipedia.org/wiki/Coronal_mass_ejection
OverviewPhysical propertiesCauseImpact on EarthAssociated phenomenaHistoryStellar coronal mass ejectionsSee also
A coronal mass ejection (CME) is a significant release of plasma and accompanying magnetic field from the Sun\'s corona into the solar wind. CMEs are often associated with solar flares and other forms of solar activity, but a broadly accepted theoretical understanding of these relationships has not been established.
---
Coronal Mass Ejections disrupt the flow of the solar wind and produce disturbances that strike the Earth with sometimes catastrophic results. The Large Angle and Spectrometric Coronagraph (LASCO) on the Solar and Heliospheric Observatory (SOHO) has observed a large number of CMEs. The event of April 7th, 1997 is shown to the left (click on the image for the animation). It produced a \"halo event\" in which the entire Sun appeared to be surrounded by the CME. Halo events are produced by CMEs that are directed toward the Earth. As they loom larger and larger they appear to envelope the Sun itself.
Coronal mass ejections are often associated with solar flares and prominence eruptions but they can also occur in the absence of either of these processes. The frequency of CMEs varies with the sunspot cycle. At solar minimum we observe about one CME a week. Near solar maximum we observe an average of 2 to 3 CMEs per day (3.4 MB MPEG movie from the SOHO/LASCO instrument showing a month of CMEs from 1998).
https://solarscience.msfc.nasa.gov/CMEs.shtml
AUTOMATIC DETECTION AND TRACKING OF CORONAL MASS EJECTIONS. II. MULTISCALE FILTERING OF CORONAGRAPH IMAGES
https://www.osti.gov/biblio/22037009-automatic-detection-tracking-coronal-mass-ejections-ii-multiscale-filtering-coronagraph-images
New Tool Could Track Space Weather 24 Hours Before Reaching Earth
https://www.nasa.gov/feature/goddard/new-tool-could-track-space-weather-24-hours-before-reaching-earth
definition:
Coronary Mass Ejection is subset of Coronal Mass Ejections,
directly targeting the Earth
subjects to study:
Aurora Borealis (Northern Lights)
Weather.gov > Sioux Falls, SD > Aurora Borealis (Northern Lights)
Current Hazards
Current Conditions
Radar
Forecasts
Rivers and Lakes
Climate and Past Weather
Local Programs
The Aurora Borealis (commonly referred to as the Northern Lights) are the result of interactions between the Sun and Earth\'s outer atmosphere. The Aurora Australis is the southern hemisphere counterpart to the Aurora Borealis.
What Causes the Aurora? The Sun emits electrically-charged particles called ions, which correspondingly move away from the Sun in a stream of plasma (ionized gas) known as the solar wind. As the plasma comes in contact with the Earth\'s magnetic field, the ions will be agitated into moving around the Earth. Some of the ions become trapped and will consequently interact with the Earth\'s ionosphere (an average of 60-80 miles above the surface), causing the ions to glow. This is the same principal as how a neon sign lights up. As electrons pass through the neon tubing, they glow, thus producing the light in a neon sign.
The Aurora are constantly changing and moving in streams of light or curtains, because the process of how the Sun\'s ionized gas interacts with the Earth\'s magnetic field is very dynamic. Although harmless to life on Earth, the Aurora can cause power disruptions in satellite communications and in radio/TV broadcasts.
Aurora Displays: The northern latitudes (or southern latitudes in the southern hemisphere) see the greatest occurrence of the Aurora. In the northern hemisphere, there is a 50% or greater chance of seeing Aurora roughly between the latitudes of 55 to 80 degrees north. This means in general that in these latitudes, the Aurora should occur on at least half of the nights throughout the year. However, this also varies. Aurora displays usually increase during times of the solar maximum. They also usually show a greater frequency during the winter months, where the nights are longer and the skies generally void of haze. Although most common in the northern latitudes, the Aurora have been occasionally seen south of 35 degrees north latitude which encompasses the far southern United States. Displays this far south can occur when a large coronal mass ejection from the Sun creates a huge geomagnetic storm in the Earth\'s outer atmosphere. This occurred on the night of November 5th and 6th, 2001 where amazing Aurora displays were seen as far south as Texas, Arizona and San Diego, CA
https://www.weather.gov/fsd/aurora
Coronal Mass Ejections
Coronal Mass Ejections (CMEs) are large expulsions of plasma and magnetic field from the Sunâs corona. They can eject billions of tons of coronal material and carry an embedded magnetic field (frozen in flux) that is stronger than the background solar wind interplanetary magnetic field (IMF) strength. CMEs travel outward from the Sun at speeds ranging from slower than 250 kilometers per second (km/s) to as fast as near 3000 km/s. The fastest Earth-directed CMEs can reach our planet in as little as 15-18 hours. Slower CMEs can take several days to arrive. They expand in size as they propagate away from the Sun and larger CMEs can reach a size comprising nearly a quarter of the space between Earth and the Sun by the time it reaches our planet.
The more explosive CMEs generally begin when highly twisted magnetic field structures (flux ropes) contained in the Sunâs lower corona become too stressed and realign into a less tense configuration â a process called magnetic reconnection. This can result in the sudden release of electromagnetic energy in the form of a solar flare; which typically accompanies the explosive acceleration of plasma away from the Sun â the CME. These types of CMEs usually take place from areas of the Sun with localized fields of strong and stressed magnetic flux; such as active regions associated with sunspot groups. CMEs can also occur from locations where relatively cool and denser plasma is trapped and suspended by magnetic flux extending up to the inner corona - filaments and prominences. When these flux ropes reconfigure, the denser filament or prominence can collapse back to the solar surface and be quietly reabsorbed, or a CME may result. CMEs travelling faster than the background solar wind speed can generate a shock wave. These shock waves can accelerate charged particles ahead of them â causing increased radiation storm potential or intensity.
Important CME parameters used in analysis are size, speed, and direction. These properties are inferred from orbital satellitesâ coronagraph imagery by SWPC forecasters to determine any Earth-impact likelihood. The NASA Solar and Heliospheric Observatory (SOHO) carries a coronagraph â known as the Large Angle and Spectrometric Coronagraph (LASCO). This instrument has two ranges for optical imaging of the Sunâs corona: C2 (covers distance range of 1.5 to 6 solar radii) and C3 (range of 3 to 32 solar radii). The LASCO instrument is currently the primary means used by forecasters to analyze and categorize CMEs; however another coronagraph is on the NASA STEREO-A spacecraft as an additional source.
Imminent CME arrival is first observed by the Deep Space Climate Observatory (DSCOVR) satellite, located at the L1 orbital area. Sudden increases in density, total interplanetary magnetic field (IMF) strength, and solar wind speed at the DSCOVR spacecraft indicate arrival of the CME-associated interplanetary shock ahead of the magnetic cloud. This can often provide 15 to 60 minutes advanced warning of shock arrival at Earth â and any possible sudden impulse or sudden storm commencement; as registered by Earth-based magnetometers.
Important aspects of an arriving CME and its likelihood for causing more intense geomagnetic storming include the strength and direction of the IMF beginning with shock arrival, followed by arrival and passage of the plasma cloud and frozen-in-flux magnetic field. More intense levels of geomagnetic storming are favored when the CME enhanced IMF becomes more pronounced and prolonged in a south-directed orientation. Some CMEs show predominantly one direction of the magnetic field during its passage, while most exhibit changing field directions as the CME passes over Earth. Generally, CMEs that impact Earthâs magnetosphere will at some point have an IMF orientation that favors generation of geomagnetic storming. Geomagnetic storms are classified using a five-level NOAA Space Weather Scale. SWPC forecasters discuss analysis and geomagnetic storm potential of CMEs in the forecast discussion and predict levels of geomagnetic storming in the 3-day forecast.
*Images courtesy of NASA and the SOHO and STEREO missions
https://www.swpc.noaa.gov/phenomena/coronal-mass-ejections
3. Tracking coronary mass ejections
Coronal Mass Ejections - NASA/Marshall Solar Physics
https://solarscience.msfc.nasa.gov/CMEs.shtml
Coronal mass ejections (or CMEs) are huge bubbles of gas threaded with magnetic field lines that are ejected from the Sun over the course of several hours. Although the Sun\'s corona has been observed during total eclipses of â¦
AUTOMATIC DETECTION AND TRACKING OF CORONAL MASS â¦
https://www.osti.gov/biblio/22037009-automatic...
20.06.2012 · Studying coronal mass ejections (CMEs) in coronagraph data can be challenging due to their diffuse structure and transient nature, and user-specific biases may be introduced through visual inspection of the images. The large amount of data available from the Solar and Heliospheric Observatory (SOHO), Solar TErrestrial RElations Observatory ...
New Tool Could Track Space Weather 24 Hours Before Reaching â¦
https://www.nasa.gov/feature/goddard/new-tool...
Jun 9, 2015 New Tool Could Track Space Weather 24 Hours Before Reaching Earth A giant cloud of solar particles, called a coronal mass ejection, explodes off the sun on Jan. 7, 2014, as seen in the light halo to the lower right in this image captured by ESA/NASA\'s Solar and Heliospheric Observatory.
Coronal mass ejection - Wikipedia
https://en.wikipedia.org/wiki/Coronal_mass_ejection
OverviewPhysical propertiesCauseImpact on EarthAssociated phenomenaHistoryStellar coronal mass ejectionsSee also
A coronal mass ejection (CME) is a significant release of plasma and accompanying magnetic field from the Sun\'s corona into the solar wind. CMEs are often associated with solar flares and other forms of solar activity, but a broadly accepted theoretical understanding of these relationships has not been established.
---
Coronal Mass Ejections disrupt the flow of the solar wind and produce disturbances that strike the Earth with sometimes catastrophic results. The Large Angle and Spectrometric Coronagraph (LASCO) on the Solar and Heliospheric Observatory (SOHO) has observed a large number of CMEs. The event of April 7th, 1997 is shown to the left (click on the image for the animation). It produced a \"halo event\" in which the entire Sun appeared to be surrounded by the CME. Halo events are produced by CMEs that are directed toward the Earth. As they loom larger and larger they appear to envelope the Sun itself.
Coronal mass ejections are often associated with solar flares and prominence eruptions but they can also occur in the absence of either of these processes. The frequency of CMEs varies with the sunspot cycle. At solar minimum we observe about one CME a week. Near solar maximum we observe an average of 2 to 3 CMEs per day (3.4 MB MPEG movie from the SOHO/LASCO instrument showing a month of CMEs from 1998).
https://solarscience.msfc.nasa.gov/CMEs.shtml
AUTOMATIC DETECTION AND TRACKING OF CORONAL MASS EJECTIONS. II. MULTISCALE FILTERING OF CORONAGRAPH IMAGES
https://www.osti.gov/biblio/22037009-automatic-detection-tracking-coronal-mass-ejections-ii-multiscale-filtering-coronagraph-images
New Tool Could Track Space Weather 24 Hours Before Reaching Earth
https://www.nasa.gov/feature/goddard/new-tool-could-track-space-weather-24-hours-before-reaching-earth