sun fact sheet

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powerpoint presentation sun fact sheet the sun is a normal g2 star, one of more than 100 billion stars in our galaxy. diameter: 1,390,000 km (earth 12,742 km or nearly 100 times smaller) mass: 1.1989 x 1030 kg (333,000 times earth’s mass) temperature: 5800 k (surface) 15,600,000 k (core) the sun contains more than 99.8% of the total mass of the solar system (jupiter contains most of the rest). chemical composition: hydrogen 92.1% helium 7.8% rest of the other 90 naturally occurring elements: 0.1% * the sun and its planets to scale * energy is created in the core when hydrogen is fused to helium. this energy flows out from the core by radiation through the radiative layer, by convection through the convective layer, and by radiation from the surface of the photosphere, which is the portion of the sun we see. * * energy from the sun passes through …

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in the structure and connections of these fields. when some of the sun's magnetic field lines are filled with hot gas, we see a magnetic loop. * the most rapid changes to the sun's magnetic field occur locally, in restricted regions of the magnetic field. however, the entire structure of the sun's global magnetic field changes on an 11 year cycle. every 11 years, the sun moves through a period of fewer, smaller sunspots, prominences, and flares - called a "solar minimum" - and a period of more, larger sunspots, prominences and flares - called a "solar maximum.“ after 11 years, when the next cycle starts, the magnetic field poles are reversed. the last solar minimum was in 2006 x-ray images of the sun taken by the yohkoh spacecraft, showing changes in the corona in 1991 (left) at a solar maximum to 1995, a solar minimum (right). * sunspots sunspots …

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of cycle on a 55- to 57-year time scale. because the pre-1700 period of low sunspot activity coincides with a prolonged cool period that is sometimes called the little ice age, some scientists have speculated that sunspot activity and climate are connected somehow. * * granules energy rises to the surface as gas wells up in the cores of the granules, and cool gas sinks around their edges. convection from inside the sun causes the photosphere to be subdivided into 1000-2000km cells. * temperature of the sun’s atmosphere * prominences are dense clouds of material suspended above the surface of the sun by loops of magnetic field. prominences can remain in a quiet or quiescent state for days or weeks. however, as the magnetic loops that support them slowly change, prominences can erupt and rise off of the sun over the course of a few minutes or hours solar prominences …

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un’s corona is forever expanding into interplanetary space filling the solar system with a constant flow of solar wind. * solar wind shapes the earth's magnetosphere and magnetic storms are illustrated here as approaching earth. these storms, which occur frequently, can disrupt communications and navigational equipment, damage satellites, and even cause blackouts. the white lines represent the solar wind; the purple line is the bow shock line; and the blue lines surrounding the earth represent its protective magnetosphere. * solar wind blows at 50-year low wednesday, 24 september 2008 14:19 uk the solar wind - the stream of charged particles billowing away from the sun - is at its weakest for 50 years. scientists made the assessment after studying 18 years of data from the ulysses satellite which has sampled the space environment all around our star. they expect the reduced output to have effects right across the solar system. …

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ion peak in the visible range. for reddish, white, and bluish-white stars, the radiation peaks lie outside the visible range. we can see such stars because they do emit some radiation in the visible range. stars as blackbody radiators * hertzsprung-russell diagram of star luminosity versus surface temperatures. the vertical axis is a comparative one based on the sun having a luminosity of 1. the horizontal axis is reversed from the normal order, with values of surface temperature increasing to the left. note that the sun is a middle-range, main-sequence star. * * thermonuclear fusion heats the inside of the star, creating pressure that stops the collapse and producing a long period of great stability that defines the main sequence. * by mass, about 70% of the sun is hydrogen. the rest is mostly 4he. hydrogen is the fuel of the nuclear reaction in the core of the sun, and …

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powerpoint presentation sun fact sheet the sun is a normal g2 star, one of more than 100 billion stars in our galaxy. diameter: 1,390,000 km (earth 12,742 km or nearly 100 times smaller) mass: 1.1989 x 1030 kg (333,000 times earth’s mass) temperature: 5800 k (surface) 15,600,000 k (core) the sun contains more than 99.8% of the total mass of the solar system (jupiter contains most of the rest). chemical composition: hydrogen 92.1% helium 7.8% rest of the other 90 naturally occurring elements: 0.1% * the sun and its planets to scale * energy is created in the core when hydrogen is fused to helium. this energy flows out from the core by radiation through the radiative layer, by convection …

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