The Sun's corona is too hot to be held back by gravity and expands radially into interplanetary space as the solar wind. The solar wind carries with it the Sun's open magnetic field as the interplanetary magnetic field (IMF). A 'southward' IMF can initiate and sustain geomagnetic activity in the forms of magnetic storms and substorms. Various high and low speed streams may be found in the solar wind which, when they interact, create complex shocks, turbulence and other features. Back to the top.

A plasma flow from the sun radiating throughout the solar system.

A stream of particles accelerated by the heat of the solar corona (outer region of the Sun) to velocities great enough to permit them to escape from the Sun's gravitational field

continuous stream of charged particles emitted by the sun in all directions.

radial outflow of hot plasma from a star's corona, carrying both mass, angular momentum, and energy away from the star

The stream of charged subatomic particles flowing steadily outward from the sun.

The constant flow of charged particles coming from the Sun in all directions

A stream of fast-moving, charged particles originating in the sun's corona and moving away from it.

Charged particles from the sun moving out in every direction at high velocity.

the plasma of charged particles(protons, electrons, and heavier ionized atoms) coming out of the Sun in all directions

a stream of electrified gas that blows from the Sun past the Earth. The solar wind blows all the time, although it is most intense during the days after a coronal mass ejection.

This is a continuous stream of matter and radiation that comes from the Sun. When a comet approaches the Sun, the effects of the solar wind can be seen as it blows the comet's tail.

The outward flow of plasma (high energy charged particles from the sun. Average speeds are about 350 km/sec. ( go to first use in the text)

An extremely rarefied gas which is streaming away from the Sun at very high speeds. Typical speeds for solar wind particles range from a couple of hundred, to several hundred, miles per second, depending upon the current state of solar 'activity'. The density of the solar wind ranges from a few dozens to a few thousands of particles per cubic inch, again depending upon the activity of the Sun. In general, the solar wind is faster and denser when the Sun is 'active', and slower and less dense when the Sun is 'quiet'.

fast wind blowing off the sun out through the Solar System.

A continuous stream of protons and electrons which is emitted by the Sun in all directions.

The solar wind does not have any noticable effects to solar power production.

The outflow of solar material from the hot, unstable corona. The solar wind blows into interplanetary space with a speed of about 400 km/s (this can vary dramatically), carrying with it the magnetic fields that originate in the Sun.

The plasma of charged particles coming out of the Sun in all directions at supersonic speeds. More about solar wind...

Streams of particles (mostly hydrogen and helium) emanating from and flowing approximately radially outward from the Sun.

Particles that move away from the sun at high speeds. The solar wind is deflected by Earth's magnetic field.

The outward flow of solar particles and magnetic fields from sun. Typically at 1 AU, solar wind velocities are near 450 km/s and proton and electron densities are near 5 cm^-3. The total intensity of the interplanetary magnetic field is nominally 5 nT. The fast solar wind originates from coronal holes and the slow wind is assumed to originate from regions near the coronal neutral line.

continuous stream of charged particles (mostly protons and electrons) ejected radially from the Sun at high velocities.

A thin flow of energetic and gas charged particles that stream from the Sun. These blow throughout the solar system at speeds of hundreds of kilometers per second.

fast-moving, charged particles (mostly protons, electrons, and helium nuclei) flowing outward from the Sun's upper atmosphere, the corona.

A Stream of energetic charged particles flowing from the Sun at a speed of about 600 km sec-1. It is the effects of the solar wind that produce aurorae in the Earth's upper atmosphere, that cause the tails of comets to stream back from the Sun, and that distort the symmetry of planetary magnetospheres.

The outflow of material from the sun's hot corona. The wind blows into space at a speed of about 800km per second (680 miles per hour), carrying with it the magnetic fields that originate in the sun.

a stream of protons moving radially from the sun

a stream of charged particles (i

a stream of charged particle s (i

a stream of charged particles which are ejected from the upper atmosphere of a star

a stream of particles leaving the suns surface and traveling through space

hot solar plasma spreading from the solar corona in all directions, at a typical speed of 300-700 km/sec. It is caused by the great heat of the corona.

A flow of charged particles (mainly protons and electrons) streaming from the Sun's outermost layer, the corona, into interplanetary space. The solar wind is extremely weak, carrying away only about 0.0001 solar masses in the course of the Sun's main sequence lifetime of about 10 billion years.

is the streams of charged particles that speed from the Sun into space.

A stream of particles, primarily electrons and protons, flowing outward from the Sun at speeds as high as 900 km/s. The solar wind is essentially the hot solar corona expanding into interplanetary and interstellar space.

The outward flux of solar particles and magnetic fields from the Sun. The solar wind is produced primarily in the cooler regions of the corona, known as coronal holes, and flows along the open magnetic field lines. Typically, solar wind velocities are 300-500 km per second.

is an outrush of ionized gas and atomic particles (protons and electrons) from the Sun. The solar wind travels at 600 to 1,000 kilometers per second and extends beyond the outer most planet. It is the action of the solar wind which keeps the tail of the comet always pointed away from the Sun.

an outward stream of electrically charged particles and radiation escaping from the Sun

The outward flux of solar particles and magnetic fields from the sun. Typically, solar wind velocities are near 215 miles/second (350 kilometers/second).

Stream of plasma, mainly electrons and protons, which flows from the Sun's corona at up to 900 km/s. It is found throughout the Solar System as far away as the heliopause. See also Heliosphere.

The hot, fast, and tenuous plasma convecting from the solar corona. Typically, the solar wind is "blowing" at 400 km/s (about a million miles per hour), has temperatures in excess of 104o K and has a density of about 10 ions and electrons per cubic centimeter. (Typical molecular densities for the atmosphere at the surface of the earth are about 1022 times larger than the solar wind density.)

a stream of ions (electrically charged atoms) emitted by the sun which meets the interstellar medium at the heliopause. At earth orbit, the solar wind averages 400 km/sec.

A fast outflow of hot gas in all directions from the upper atmosphere of the Sun ("solar corona"), which is too hot to allow the Sun's gravity to hold on to its gas. Its composition matches that of the Sun's atmosphere (mostly hydrogen) and its typical velocity is 400 km/sec, covering the distance from Sun to Earth in 4-5 days. The solar wind confines the Earth's magnetic field inside a cavity known as the magnetosphere and supplies energy to phenomena in the magnetosphere such as polar aurora ("northern lights") and magnetic storms.

A continuous wind of charged particles from the sun, blowing through interplanetary space.

A current of charged particles that streams outward from the Sun.

A stream of charged particles emitted from the Sun which travel into space along lines of magnetic flux.

A stream of high-speed, ionized particles ejected primarily from the Sun.

The wind from the Sun. More specifically, particles, usually electrons and protons, continually streaming away from the corona of the Sun. The solar wind is extremely sparse, containing only a few fast moving particles per cubic centimeter at the Earth. The exact geometry and extent of the solar wind is not well known.

Plasma that come out of the Sun in all directions at very fast speeds.

A stream of particles with enough energy to escape from the Sun's gravity and flow outward into space.

the stream of charged subatomic particles emanating from the sun

Ions of gas which stream rapidly away from the Sun. The solar wind follows the magnetic field of the Sun out through the solar system in a slightly spiral path.

A flow of charged particles that travels from the Sun out into the solar system.

tenuous flow of gas and energetic charged particles, mostly protons and electrons which stream from the sun. They are usually near 350 kilometers per second.

a very hot gas that is being blown away from the Sun at a high speed.

A flow of hot charged particles leaving the Sun.

A continuous stream of charged particles which are released from the Sun and hurled outward into space at speeds up to 800 kilometers per second. Solar winds are very prominent after solar flare activity.

A supersonic outflow of plasma from the Sun that fills interplanetary space and produces the antisunward tails of comets and planetary magnetospheres.

The solar wind is a continuous stream of ions (electrically charged particles) that are given off by the sun. Since the particles are emitted from the Sun as the Sun rotates, the solar wind blows in a pinwheel pattern through the solar system. It takes the solar wind about 5 days to reach Earth; it has a velocity of about 500 miles/hour (800 km/sec). The solar wind travels along vibrating magnetic waves which are propagated by the Sun

continuous outflow of plasma from the solar atmosphere (corona) into the solar system

The outward flow of charged particles from the sun into space. (TOP OF THE PAGE) (CLOSE WINDOW)

Streams of particles (mostly ions of hydrogen and helium, and electrons ) emanating from the Sun and flowing approximately radially outward at velocities from 300 to 800 km per sec.

a high-speed flow of low-density electrical particles, mainly electrons and protons, emitted by the sun in all directions into space. The speed of the solar wind varies from about 200 to 1000 miles per second, so takes between one and five days to reach the Earth.

The charged particles (plasma), primarily protons and electrons, that are continuously emitted from the Sun and stream outward throughout the solar system at speeds of hundreds of kilometers per second.

The hot, fast, and tenuous plasma convecting from the solar corona. Typically, the solar wind is "blowing" at 400 km/s, has temperatures in excess of 100000 K, and has a density of about 10 ions and electrons per cubic centimeter. (For comparison, water boils at about 373 K. Typical molecular densities for the atmosphere at the surface of Earth are about 1022 times larger than the solar wind density.) See also: Ever-Changing Sun Causes Space Weather

a flux of charged particles (plasma) emitted by the Sun or by a star.

A stream of charged particles, mostly protons and electrons, that escapes into the Sun's outer atmosphere at high speeds and streams out into the solar system.

A tenuous flow of gas and energetic charged particles, mostly protons and electrons -- plasma -- which stream from the Sun; typical solar wind velocities are almost 350 kilometers (217 miles) per second.

A stream of energetic, charged particles of matter (mostly electrons and light-element ions) that constantly escape the Sun, thereby bathing much of the Solar System in an extended solar atmosphere or "heliosphere."

Solar wind is the plasma coming out of the Sun in all directions at very high speeds -- an average of about 400 km/sec, almost a million mph! Solar Wind is responsible for the tails of comets pointing away from the Sun and the shape of the magnetic fields around the planets. Solar wind can also have a measurable effect on the flight paths of spacecraft. This image of Comet Hale-Bopp is courtesy of Fred Espenak, NASA GSFC. The Sun would be to the right of the comet. The solar wind pushes the tail to the left.

charged particles from the sun traveling at about 1.5 million kph.

Stream of ionized gas, mainly hydrogen, continuously flowing outward from the sun, at very high velocity (≈ 400 km s−1 on the average) and with variable intensity. While passing near the earth the solar wind interacts with the magnetic field to produce various effects in the upper atmosphere (e.g., aurora).

Rapidly moving atoms and ions that escape from the solar corona and blow outward through the solar system.

Streams of charged particles flowing from the Sun at millions of kilometers per hour. This high-speed solar wind varies in composition, always streams away from the Sun, and interacts with other regions of matter in the solar system.

A stream of tiny particles of gas and plasma emitted by the Sun. The speed of the solar wind is about 400 kilometers (250 miles) per second in the vicinity of Earth's orbit.

Solar Wind is a British small press comicbook. Edited by Cosmic Ray (a pseudonym for small press comics publisher Paul Scott), the comic is devoted to gentle parodies of British boys' comics of the 1970's and 80's.