From Simple English Wikipedia, the free encyclopedia

The heliosphere is the magnetosphere, stellar wind bubble and outermost atmospheric layer of the Sun.

Diagram of features of the heliosphere. Based on preliminary results from the Interstellar Boundary Explorer.

The heliosphere is the cavity made by the Sun in the interstellar medium. Almost all of the material in the heliosphere comes from the Sun itself.

For the first ten billion kilometres of its radius, the solar wind travels at over a million kilometres per hour.[1][2] It slows down before finally stopping altogether. The point where the solar wind slows down is the termination shock; the point where the interstellar medium and solar wind pressures balance is called the heliopause; the point where the interstellar medium, travelling in the opposite direction, slows down as it collides with the heliosphere is the bow shock.

Solar wind[change | change source]

The solar wind is made of particles. They are charged (ionized) atoms from the solar corona, and fields, in particular magnetic fields. As the Sun rotates once in about 27 days, the magnetic field transported by the solar wind gets wrapped into a spiral. Differences in the Sun's magnetic field are carried outward by the solar wind and can produce magnetic storms in the Earth's magnetosphere.

In March 2005, measurements by the Solar Wind Anisotropies (SWAN) instrument onboard the Solar and Heliospheric Observatory (SOHO) showed that the heliosphere, the solar wind-filled volume which prevents the solar system from becoming embedded in the local (ambient) interstellar medium, is not axisymmetrical, but is distorted, very likely under the effect of the local galactic magnetic field.[3]

References[change | change source]

  1. Dr. David H. Hathaway (January 18, 2007). "The Solar Wind". NASA. Archived from the original on 2015-08-13. Retrieved 2007-12-11.
  2. Britt, Robert Roy (March 15, 2000). "A Glowing Discovery at the Forefront of Our Plunge Through Space". SPACE.com. Archived from the original on 2001-01-11. Retrieved 2006-05-24.
  3. Lallement, R.; Quémerais, E.; Bertaux, J. L.; Ferron, S.; Koutroumpa, D.; Pellinen, R. (2005). "Deflection of the Interstellar Neutral Hydrogen Flow Across the Heliospheric Interface". Science. 307 (5714): 1447–1449. Bibcode:2005Sci...307.1447L. doi:10.1126/science.1107953. PMID 15746421. S2CID 36260574. Retrieved 2007-05-25.{{cite journal}}: CS1 maint: multiple names: authors list (link)