RECENT NASA OBVSERVATIONS OF FLARE1080

June 6/2010-4:53 PM EST
   By : Isaac N.

   Lighting just hit a boat in the Gulf. There are massive rainstorms, lightening and flooding everywhere. There are very deep powerful earthquakes under Cuba Sumatra, and California among others in the past 5 days, important because deep movements signify larger forces than normal at play. The cause is sunspot 1080. NASA observed it happening over the past week and a half. It is responsible for the weather and the movements in the earths crust.

Here's how it works.



Solar flares influence and charge our ionosphere.

Our ionosphere influences our magnetosphere.

Our magnetosphere controls tectonic movements...

The whole Gulf is salt.

   High amounts of ferromagnetic salt in the Sigsbee. If you work in the petroleum industry you know about salt types and magnetism, as well as the geoscientific studies of the sun-cycles.

   Big solar flares cause earthquakes.

   Even slight tectonic movements cause raised pressure in oil fields.

   Sudden raises in pressures cause blowouts.

    As far as toxic gases in the Gulf, and they interplay between them, salt and the sun, look up whats known as a gas diffusion electrode.

  Gas diffusion electrodes (GDE) are electrodes with a conjunction of a solid, liquid and gaseous interface, and an electrical conducting catalyst supporting an electrochemical reaction between the liquid and the gaseous phase

   BTW, these things I am telling you about are all commonly accepted facts in the world of geomagnetic sciences and astrophysics, among others.

 There are many important events happening at the same time, that's what is accounting for eveything we are seeing..

They are reciprocal self-feeding cycles when in conjunction. Modern science can only start to guess what will happen in the next 30 days on this planet.

Solar flares disrupt the ionosphere, but also charge it up, that accounts for the lightning you are seeing everywhere.

Below is the scientific stuff,  if you are interested.


   The ionosphere has several layers created at different altitudes and made up of different densities of ionization. Each layer has its own properties, and the existence and number of layers change daily under the influence of the Sun. During the day, the ionosphere is heavily ionized by the Sun. During the night hours the cosmic rays dominate because there is no ionization caused by the Sun (which has set below the horizon). Thus there is a daily cycle associated with the ionizations.

   In addition to the daily fluctuations, activity on the Sun can cause dramatic sudden changes to the ionosphere. The Sun can unexpectedly erupt with a solar flare, a violent explosion in the Sun's atmosphere caused by huge magnetic activity. These sudden flares produce large amounts of X-rays and EUV energy, which travel to the Earth (and other planets) at the speed of light.

http://sid.stanford.edu/activities/activity.html

  Next....

here's how solar flares influence the ionosphere.

   Data from NASA's Imager for Magnetopause to Aurora Global Exploration (IMAGE) satellite show that two parallel bands of ionized particles that encircle the Earth in the tropics are altered by persistent storms over the Amazon Basin in South America, the Congo Basin in Africa, and Indonesia. The net effect of these repeated storms is to create a denser region of ionospheric plasma over these areas that glows more brightly in ultraviolet light than does the rest of the two plasma bands.

   "This discovery will help improve forecasts of turbulence in the ionosphere, which can disrupt radio transmissions and the reception of signals from the Global Positioning System," said Thomas Immel, an assistant research physicist at UC Berkeley's Space Sciences Laboratory and lead author of a paper on the research published Aug. 11 in Geophysical Research Letters.

   The ionosphere is formed by solar x-rays and ultraviolet light, which break apart atoms and molecules in the upper atmosphere, creating a layer of ionized, or electrically-charged, gas known as plasma. The densest part of the ionosphere forms two bands of plasma close to the equator at a height of almost 250 miles.

  From March 20 to April 20, 2002, a period when the IMAGE satellite flew low over the tropics, on-board sensors recorded these bands, which glow in ultraviolet light. The pictures showed four pairs of bright bulges in the bands where the ionosphere was almost twice as dense as the average. Three of the bright pairs were located over tropical rainforests with lots of thunderstorm activity - the Amazon Basin in South America, the Congo Basin in Africa, and Indonesia. A fourth pair appeared over the Pacific Ocean.

The connection between thunderstorms and plasma bands in the ionosphere at first seemed unlikely, because the gas in the ionosphere is simply too thin for atmospheric tides to directly affect the much higher ionosphere. Thunderstorms develop in the lower atmosphere, or troposphere, which extends almost 10 miles above the equator. The gas in the plasma bands, 250 miles up, is about 10 billion times less dense than in the troposphere. The tide would have to collide with atoms in the atmosphere above to propagate upward, but the ionosphere where the plasma bands form is so thin, atoms rarely collide.

   To get an idea of what might be happening, Immel and his UC Berkeley colleagues modeled the atmospheric tides using a computer simulation, called the Global Scale Wave Model, developed by the National Center for Atmospheric Research in Boulder, Colo.

   The simulation showed that the tides could affect the plasma bands indirectly by modifying a layer of the atmosphere below the bands that shape them. Below the plasma bands, a layer of the ionosphere called the E-layer becomes partially electrified during the day. This region creates the plasma bands above it when high-altitude winds blow plasma in the E-layer across the Earth's magnetic field. Since plasma is electrically charged, its motion across the Earth's magnetic field acts like a generator, creating an electric field. This electric field shapes the plasma above into the two bands. that would change the motion of the E-layer plasma and also would also change the electric fields it generates, which would then reshape the plasma bands above.

     The Global Scale Wave Model indicated the tides should dump their energy, released when water condenses into clouds, about 62 to 75 miles above the Earth in the E-layer. This is high enough to disrupt the plasma currents there, altering the electric fields and creating dense, bright zones in the plasma bands above.

"The single pair of bright zones over the Pacific Ocean that is not associated with strong thunderstorm activity shows the disruption is propagating around the Earth, making this the first global effect on space weather from surface weather that's been identified," said Immel. "We now know that accurate predictions of ionospheric disturbances have to incorporate this effect from tropical weather."

"This discovery has immediate implications for space weather, identifying four sectors on the Earth where space storms may produce greater ionospheric disturbances. North America is in one of these sectors, which may help explain why the U.S. suffers uniquely extreme ionospheric conditions during space weather events," he added.

    Measurements made by NASA's Thermosphere Ionosphere Mesosphere Energetics and Dynamics (TIMED) satellite from March 20 to April 20, 2002, have confirmed that the dense zones exist in the plasma bands. Researchers now want to understand whether the effect changes with seasons or large events, like hurricanes.

    The research was funded by NASA. The National Center for Atmospheric Research is sponsored by the National Science Foundation.

http://www.berkeley.edu/news/media/releases/2006/09/14_weather.shtml


Next, here's what the influence of the ionosphere is on the geomagnetic forces in the earths crust..


    The geomagnetic field has a regular small variation with a fundamental period of 24 hours. This variation is easiest to observe during periods of low solar activity when large irregular disturbances are less frequent (see section 3.7 below). For this reason it is often referred to as the Solar quiet or Sq variation. Figure 8 shows the actual variation in declination recorded at Hartland observatory on June 22nd, 2004. This graph is typical of the smooth Sq variation seen at this latitude. Below this is the variation in a compass needle at Hartland over the same period. In reality, this type of variation in the geomagnetic field would affect the direction of a compass needle by no more than a few tenths of a degree. Inclination varies by less than a tenth of a degree and the total intensity of the magnetic field is perturbed by only a few tens of nT, which represents about 0.1% of the Earth's magnetic field strength at Hartland. Although these effects are very small, they can be of interest to those who use measurements of the Earth's magnetic field as a tool for very precise navigation


The field arising from magnetic materials in the Earth's crust varies on all spatial scales and is often referred to as the anomaly field. A knowledge of the crustal magnetic field is often very valuable as a geophysical exploration tool for determining the local geology.

    The anomalies seen at mid-ocean spreading ridges are of particular interest. At these locations molten mantle comes to the surface and solidifies to form new oceanic crust, preserving in it the strength and direction of the contemporary ambient magnetic field. As new material is extruded, the existing crust is pushed away on either side of the ridge, with the direction of the ambient magnetic field at time of formation frozen into it. Marine and aeromagnetic surveys reveal a series of stripes in the total intensity anomalies which run parallel to and symmetrically about the central ridge and these are interpreted as alternating blocks of normal and reversely magnetized oceanic crust. This discovery of a crude tape recorder of the Earth's magnetic field and its reversals was invaluable to the theory of plate tectonics developed in the 1960s.

The Earth's magnetic field is generated in the fluid outer core by a self-exciting dynamo process. Electrical currents flowing in the slowly moving molten iron generate the magnetic field. In addition to sources in the Earth's core the magnetic field observable at the Earth's surface has sources in the crust and in the ionosphere and magnetosphere. The geomagnetic field varies on a range of scales and a description of these variations is now made, in the order low frequency to high frequency variations, in both the space and time domains. The final section describes how the Earth's magnetic field can be both a tool and a hazard to the modern world. First of all, however, methods of observing the magnetic field are described.
    The Earth's magnetic field is observed in a number of other ways. These are repeat stations and surveys made on land, from aircraft and ships. Repeat stations are permanently marked sites where high-quality vector observations of the Earth's magnetic field are made for a few hours, sometimes a few days, every few years. Their main purpose is to track changes in the core-generated magnetic field.

    Most aeromagnetic surveys are designed to map the crustal field. As a result they are flown at altitudes lower than 300 m, they cover small areas, generally once only, with very high spatial resolution. Because of the difficulty in making accurately oriented measurements of the magnetic field on a moving platform, these kinds of aeromagnetic surveys generally comprise total intensity data only. However, between 1953 and 1994 the Project MAGNET programme collected high-level three-component aeromagnetic data specifically for modelling the core-generated field. The surveys were mainly over the ocean areas of the Earth, at mid to low latitudes. A variety of platforms and instrumentation were used; the most recent set-up included a fluxgate vector magnetometer mounted on a rigid beam in the magnetically clean rear part of the aircraft, a ring laser gyro fixed at the other end of the beam, and a scalar magnetometer located in a stinger extending some distance behind the aircraft's tail section.

Modern marine magnetic surveys are also invariably designed to map the crustal field but with careful processing it is possible to obtain information about the core-generated field from the data. In a marine magnetic survey a scalar magnetometer is towed some distance behind a ship, usually along with other geophysical equipment, as it makes either a systematic survey of an area or traverses an ocean.


The present magnetic field

    In a source-free region near the surface of the Earth the magnetic field is the negative gradient of a scalar potential which satisfies Laplace's equation. A solution to Laplace's equation in spherical coordinates is called a spherical harmonic expansion and its parameters are called Gauss coefficients. There are internal or external coefficients, modeling the field generated inside or outside the Earth respectively. A separation of the core and crustal fields, both internal, is not perfect. The internal field is often called the main field.


Westward drift

   Using direct observations of the magnetic field over the past 400 years, the pattern of declination seen at the Earth's surface appears to be moving slowly westwards. This is particularly apparent in the Atlantic hemisphere at mid- and equatorial latitudes. This may be related to the motion of fluid at the core surface slowly westwards, dragging with it the magnetic field lines.

Crustal magnetic field

   The field arising from magnetic materials in the Earth's crust varies on all spatial scales and is often referred to as the anomaly field. A knowledge of the crustal magnetic field is often very valuable as a geophysical exploration tool for determining the local geology.

   The anomalies seen at mid-ocean spreading ridges are of particular interest. At these locations molten mantle comes to the surface and solidifies to form new oceanic crust, preserving in it the strength and direction of the contemporary ambient magnetic field. As new material is extruded, the existing crust is pushed away on either side of the ridge, with the direction of the ambient magnetic field at time of formation frozen into it. Marine and aeromagnetic surveys reveal a series of stripes in the total intensity anomalies which run parallel to and symmetrically about the central ridge and these are interpreted as alternating blocks of normal and reversely magnetised oceanic crust. This discovery of a crude tape recorder of the Earth's magnetic field and its reversals was invaluable to the theory of plate tectonics developed in the 1960s.

      Field variations at quiet times

   The geomagnetic field has a regular small variation with a fundamental period of 24 hours. This variation is easiest to observe during periods of low solar activity when large irregular disturbances are less frequent (see section 3.7 below). For this reason it is often referred to as the Solar quiet or Sq variation. Figure 8 shows the actual variation in declination recorded at Hartland observatory on June 22nd, 2004. This graph is typical of the smooth Sq variation seen at this latitude. Below this is the variation in a compass needle at Hartland over the same period. In reality, this type of variation in the geomagnetic field would affect the direction of a compass needle by no more than a few tenths of a degree. Inclination varies by less than a tenth of a degree and the total intensity of the magnetic field is perturbed by only a few tens of nT, which represents about 0.1% of the Earth's magnetic field strength at Hartland. Although these effects are very small, they can be of interest to those who use measurements of the Earth's magnetic field as a tool for very precise navigation

   This regular fluctuation is caused by electrical currents high in the ionosphere, a region that begins at an altitude of about 100 km. All currents, like those in wires, can only flow in materials that conduct. The copper used in wires conducts very well but the air is a poor conductor. However, in the ionosphere high energy ultra-violet rays and X-rays from the Sun displace electrons from (or ionise) the neutral (uncharged) molecules in the air to produce positive and negatively charged particles (see Figure 9, '+' and '-' represent the charged particles). These charges allow the air to conduct. At any point on Earth, the Sun is at its most intense around midday and is therefore generating the most charges in the ionosphere overhead, which allows the air to conduct better. After dusk, in the absence of ionising radiation, the charges begin to recombine into neutral molecules again and so the ability for the air to conduct is reduced. This cycle is repeated each day.

    The sunlight not only makes the air conduct, it also heats it causing thermo-tidal winds. These winds combine with the tidal winds caused by the gravitational pull of the Sun and Moon and drive the ionospheric dynamo. This dynamo generates currents as the conducting ionosphere is driven through the Earth's magnetic field. These current systems form two closed loops: an anti-clockwise vortex in the northern hemisphere and a clockwise vortex in the southern hemisphere, like those shown in Figure 10. Because it is solar radiation that produces the charges that in turn let the atmosphere conduct, the currents remain predominantly on the sunlit side of the Earth. It is these currents that produce the daily magnetic field fluctuations as the Earth rotates beneath, which explains why the magnetic field varies throughout the day. The shape, size and location of these vortices also explain why the Sq variation depends on latitude. As the amount of solar radiation falling upon the northern and southern hemispheres varies with the seasons and solar cycle, the Sq variation also varies.
    As well as the regular daily variation the Earth's magnetic field also exhibits irregular disturbances, and when these are large they are called magnetic storms. These disturbances are caused by interaction of the solar wind, and disturbances therein, with the Earth's magnetic field. The solar wind is a stream of charged particles continuously emitted by the Sun and its pressure on the Earth's magnetic field creates a bounded comet-shaped region surrounding the Earth called the magnetosphere. When there is a disturbance in the solar wind the current systems existing within the magnetosphere are enhanced and cause magnetic disturbances and storms. Figure 8 shows a schematic picture of the solar wind and the Earth's magnetosphere.
   The amplitude of magnetic disturbances is larger at high latitudes because of the presence of the oval bands of enhanced currents around each geomagnetic pole called auroral electrojets. Some charged particles get trapped at the boundary of the magnetosphere and, in the polar regions, are accelerated along the magnetic field lines towards the atmosphere and finally colliding with oxygen and nitrogen molecules. These collisions result in sometimes spectacular emissions of mainly red and green light known as aurora borealis at northern latitudes and aurora australis at southern latitudes.

The prevailing conditions in the solar-terrestrial environment which are a consequence of the emission of charged particles from the Sun and their interaction with the Earth's magnetic field, is called space weather. There is presently some considerable interest in forecasting space weather and data from satellites observing the Sun and the solar wind are extremely valuable for this.

    Although irregular, magnetic disturbances exhibit some patterns in their frequency of occurence. The main pattern is the correlation with the 11-year solar cycle and Figure 9 shows the number of magnetic storms per year, from 1868 to present and the corresponding number of sunspots. Another important pattern is the 27-day recurrence of some storms related to the 27-day rotation of the Sun as seen from Earth.


   The annual number of magnetic storms is represented by each bar of the histogram. Superimposed is the smoothed sunspot number. The dashed lines indicate solar minima and the dotted lines indicate solar maxima. Note the correlation of magnetic activity with solar activity and the apparent increase in magnetic activity with time.

A specialist form of navigation is directional drilling in the petroleum industry. There are two main methods of navigation available for drilling deviated wells towards often small targets in the oil reservoirs. One method makes use of gyro tools but this can be expensive. The other method makes use of magnetic tools. As accuracy is critical for economic reasons and to avoid well collisions, the accuracy requirements on the Earth's magnetic field values, used to correct the direction of the well from magnetic bearings to true bearings, are typically 0.1° in direction and 50 nT in total intensity. To attain these accuracies account must be taken of the crustal field, daily variations and magnetic storms. This application is an example of the Earth's magnetic field being a tool in the modern world but it can also be a hazard if no account is taken of these other sources.

Solar wind and the Earth's magnetosphere.

The amplitude of magnetic disturbances is larger at high latitudes because of the presence of the oval bands of enhanced currents around each geomagnetic pole called auroral electrojets. Some charged particles get trapped at the boundary of the magnetosphere and, in the polar regions, are accelerated along the magnetic field lines towards the atmosphere and finally colliding with oxygen and nitrogen molecules. These collisions result in sometimes spectacular emissions of mainly red and green light known as aurora borealis at northern latitudes and aurora australis at southern latitudes.

The prevailing conditions in the solar-terrestrial environment which are a consequence of the emission of charged particles from the Sun and their interaction with the Earth's magnetic field, is called space weather. There is presently some considerable interest in forecasting space weather and data from satellites observing the Sun and the solar wind are extremely valuable for this.

Although irregular, magnetic disturbances exhibit some patterns in their frequency of occurence. The main pattern is the correlation with the 11-year solar cycle and Figure 9 shows the number of magnetic storms per year, from 1868 to present and the corresponding number of sunspots. Another important pattern is the 27-day recurrence of some storms related to the 27-day rotation of the Sun as seen from Earth.

 The bands of the ionosphere that is influenced most.

 Images below were from the recent flare

 Here is IRIS earthquake browser screen shot of the latest activities around the world.

So that's how it works.

http://sid.stanford.edu/activities/activity.html

http://www.agu.org/meetings/ja08/ja08-sessions/ja08_T33A.html

http://www.geomag.bgs.ac.uk/earthmag.html#_Toc2075559

http://www.berkeley.edu/news/media/releases/2006/09/14_weather.shtml

























These movement are all the same plate trying to move, notice the depth and magnitude. Same thing in Cuba and Cali.