güneş rüzgarı

Türkisch - Englisch

Definition von güneş rüzgarı im Türkisch Englisch wörterbuch

(Astronomi) solar wind

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

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

The flow of charged particles around the suns corona

A stream of high-speed, ionized particles ejected primarily from the sun's corona. Flux of particles, chiefly protons, electrons, and helium nuclei accelerated by the hot solar corona's high temperatures to speeds high enough to allow them to escape the Sun. Solar flares increase its intensity. The solar wind deflects planets' magnetospheres and the ion tails of comets away from the Sun. The uninterrupted portion of the solar wind continues to travel to a distance of about 20 astronomical units, where it cools and eventually diffuses into interstellar space. See also heliopause

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

a stream of protons moving radially from the sun

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 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 centimetre at the Earth The exact geometry and extent of the solar wind is not well known

Solar wind is the name astronomers use for the steady stream of particles (mostly hydrogen and helium ions and electrons) that flows away from the Sun at all times The solar wind is very dilute: In a laboratory on Earth it would be considered a vacuum You can see the solar wind in the Corona Image Map

The outward flow of solar particles and magnetic fields from the Sun Typically at 1 AU, solar wind velocities are near 375 km/s and proton and electron densities are near 5 per cubic centimeter The total intensity of the interplanetary magnetic field is nominally 5 nT

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

A continuous plasma stream expanding into interplanetary space from the sun's corona The solar wind is present continuously in interplanetary space After escaping from the gravitational field of the sun, this gas flows outward at a typical speed of 400 km per second to distances known to be beyond the orbit of Pluto Besides affecting Earth's weather, solar activity gives rise to a dramatic visual phenomena in our atmosphere The streams of charged particles from the Sun interact the Earth's magnetic field like a generator to create current systems with electric potentials of as much as 100,000 volts Charged electrons are energized by this process, sent along the magnetic field lines towards Earth's upper atmosphere, excite the gases present in the upper atmosphere and cause them to emit light which we call the auroras The auroras are the northern (aurora borealis) and southern (aurora Australis) lights

The outflow of charged particles from the solar corona into space Because of the high temperature of the particles (mostly protons and electrons) of the corona, they are moving at speeds higher than the solar escape velocity At the orbit of the Earth, these particles are moving at about 500 km/sec Some of these particles are captured by the magnetic fields of the planets, forming their magnetospheres

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

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 flow of gas and energetic charged particles, mostly protons and electrons -- plasma -- which stream from the Sun; typical solar wind velocities are near 350 kilometers per second

a stream of particles flowing from the Sun

a constant flow of electromagnetic radiation and charged particles, mostly protons and electrons, from the Sun

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

Silbentrennung

gü·neş rüz·ga·rı