SCAREY STUFF. Class M-4.8 Coronal Mass Ejection (CME) Projected Directly at Earth 06:10 UTC 28/08/2021

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What causes Yellowstone Earthquake Swarms: https://www.usgs.gov/center-news/what-causes-earthquake-swarms-yellowstone

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Solar Monitoring:

Bt/Bz (white/red lines) - Bt indicates the total strength of the Interplanetary Magnetic Field (IMF) carried by the solar wind. A higher number indicates a stronger impact to earth's magnetic field. Bz indicates the orientation of the IMF. If the Bz is positive (northward), then the earth's magnetic field will block most of the solar wind, and geomagnetic storming is unlikely. But if Bz is negative (southward), then the sun and the earth's magnetic field will link up, which allows the solar wind to pour into the earth's atmosphere, causing the aurora. The further southward the Bz points and the longer the duration, the higher the chance is of a geomagnetic storm occurring.

Phi (blue line) - Phi is the angle of the IMF measured in the GSM (geocentric solar magnetospheric) coordinate system. Sudden and rapid changes in the Phi angle in conjunction with increased solar wind speeds and Bz fluctuations is common during a CME impact.

Density (orange line) - The solar wind carries with it plasma (electrons and protons). This is measured in atoms per cubic centimeter. A high and fluctuating plasma density is usually better at stirring up the aurora.

Speed (yellow line) - Measured in kilometers per second, the speed of the solar wind can vary from 250 - 800+ km/s. A faster solar wind is usually associated with elevated geomagnetic activity.

Temp (green line) - Measured in Kelvin units. A rise in temperature is likely during an impact to earth's magnetic field.
C2 images show the inner solar corona up to 8.4 million kilometers (5.25 million miles) away from the Sun.

C3 images have a larger field of view: They encompass 32 diameters of the Sun. To put this in perspective, the diameter of the images is 45 million kilometers (about 30 million miles) at the distance of the Sun, or half of the diameter of the orbit of Mercury. Many bright stars can be seen behind the Sun.

EIT (Extreme ultraviolet Imaging Telescope) images the solar atmosphere at several wavelengths, and therefore, shows solar material at different temperatures. In the images taken at 304 Angstrom the bright material is at 60,000 to 80,000 degrees Kelvin. In those taken at 171 Angstrom, at 1 million degrees. 195 Angstrom images correspond to about 1.5 million Kelvin, 284 Angstrom to 2 million degrees.

The MDI (Michelson Doppler Imager) images shown here are taken in the continuum near the Ni I 6768 Angstrom line. The most prominent features are the sunspots. This is very much how the Sun looks like in the visible range of the spectrum. The magnetogram image shows the magnetic field in the solar photosphere, with black and white indicating opposite polarities.

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The University of Michigan’s BATS-R-US magnetohydrodynamic (MHD) model of the magnetosphere

Courtesy of NASA/SDO/Goddard Space Flight Center and the AIA, EVE, and HMI science teams.

SWPC images and animations from GOES SUVI instruments in near-real-time, for analyzing and observing events.

This work utilizes SOLIS data obtained by the NSO Integrated Synoptic Program (NISP), managed by the National Solar Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation.

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