Latest Solar flare Stories
New research from an international team of researchers using NASA's Fermi telescope reports the first-ever gamma ray study of the cosmic phenomenon.
The sun ushered out 2013 and welcomed 2014 with two mid-level flares on Dec. 31, 2013 and Jan. 1, 2014.
A new NASA movie of the sun based on data from NASA's Solar Dynamics Observatory, or SDO, shows the wide range of wavelengths – invisible to the naked eye – that the telescope can view. SDO converts the wavelengths into an image humans can see, and the light is colorized into a rainbow of colors.
The Geostationary Operational Environmental Satellite – R known as GOES-R Series Program completed its next instrument, SUVI or the Solar Ultra-Violet Imager, which is now ready for integration onto the GOES-R spacecraft.
Adding on to a series of solar flares throughout October and November, the sun emitted another significant solar flare on Nov. 19, 2013, peaking at 5:26 a.m. EST.
Two large, complex sunspots are moving across the face of the sun.
The sun emitted a significant solar flare that peaked at 1:14 a.m. EST on Nov. 10, 2013.
A key instrument that will fly on the Geostationary Operational Environmental Satellite – R (GOES-R) spacecraft, NOAA’s next-generation of geostationary satellites, is cleared for installation on the spacecraft.
The sun emitted a significant solar flare – its fourth X-class flare since Oct. 23, 2013 -- peaking at 5:54 p.m. on Oct. 29, 2013.
Photosphere -- The photosphere of an astronomical object is the region at which the optical depth becomes one. In other words, the photosphere is the place where an object stops being transparent. It is typically used to describe the Sun or another star. Because stars are large balls of gas, they have no solid surface. However, there is a depth at which the gas stops being transparent to photons, and this depth provides a visual surface to the star. The Sun's photosphere has a...
Corona -- The corona is the luminous "atmosphere" of the Sun extending millions of kilometers into space, most easily seen during a total solar eclipse. An interesting feature of the corona is the fact that it is much hotter than the visible "surface" of the Sun; the photosphere is approximately 6000°C compared to the corona at over one million °C. The corona is much less dense than the photosphere, however, and so produces less light. The exact mechanism by which the corona is...
Chromosphere -- The chromosphere (literally, "color sphere") is a thin layer of the Sun's atmosphere just above the photosphere, roughly 10,000 kilometers deep. The chromosphere is more visually transparent than the photosphere. The most common solar feature within the chromosphere are spicules, long thin fingers of luminous gas which appear like the blades of a huge field of fiery grass growing upwards from the photosphere below. Spicules rise to the top of the chromosphere and then sink...
Solar Wind -- Solar wind, a stream of particles (mostly high-energy protons ~ 500 Kev) that is continually ejected from the surface of the Sun. The composition of this plasma is identical to the Sun's corona, 73% hydrogen and 25% helium with the remainder as trace impurities, and is ionized. Near Earth, the velocity of the solar wind varies from 200km/s-889km/s. The average is 450 km/s. Approximately 3000 tons of material is lost from the Sun every hour as solar wind. Since solar...
Solar Maximum -- The Sun, a roiling ball of plasma, occupies its place in space approximately 93 million miles from Earth. Though it seems simple to inhabitants of this planet -- the Sun shines, giving light and heat -- the processes occurring in the Sun are so complex that many scientists devote their careers to just one aspect of solar activity. Changes in the activity of the Sun particularly engage solar scientists. Whether fluctuations in the solar magnetic field, expulsions of...
- Forsooth! indeed! originally a parenthetical phrase used in repeating the words of another with more or less contempt or disdain.