This science game helps in learning more about sun. The sun is a stellar body composed of hydrogen, oxygen and helium. Hydrogen makes up three-quarters of the sun, and helium makes up almost the entire remaining quarter. Other gases and metals comprise the remaining 1.69 percent of the sun's mass. These include iron, oxygen, silicon, sulfur, carbon, neon, calcium, chromium, and magnesium. In addition to hydrogen and helium, the sun also contains traces of carbon, nitrogen, sulfur and magnesium.
Elements in the Sun
The Sun is mostly hydrogen and helium, with a few other trace elements. It contains about one percent "dirt" and 67 known chemical elements. The abundance of each of these elements is listed below. Hydrogen makes up approximately ninety percent of the mass of the Sun, and helium makes up the remaining twenty-seven percent. Other elements, such as phosphorus, uranium, and nitrogen, are found in trace amounts and make up less than one percent of the mass of the Sun.
The Sun is the star at the center of our Solar System. It is a nearly perfect ball of hot plasma that is heated to incandescence by nuclear fusion reactions in its core. The Sun radiates energy as visible light, ultraviolet light, and infrared radiation, and is the primary source of energy for life on Earth. However, it is not the only source of energy. The Sun is a great example of how far we can see it and how much it can light up our planet.
The composition of the Sun has long baffled scientists. The solar spectrum contains 67 elements, with hydrogen and helium making up 98% of its mass. The spectral line that stretches from the chromosphere to the surface is the "photosphere," the region where light strikes the solar surface. These spectra are not representative of the entire solar interior, though, and the Sun's magnetic field may not be constant throughout its whole lifetime.
The polar crown gaps and polarity reversals on the solar surface have been studied in detail. A decade-long stack plot is able to show the evolution of polar crown gaps and polarity reversals. This analysis of solar surface features allows the study of changes in polarity and longitudinal drifts. Several studies have also linked the evolution of the magnetic field of the Sun to eruptions, space weather, and solar wind streams.
Scientists study solar flares with particular interest. Solar flares are explosions of energy that produce shockwaves on the surface of the Sun. They occur when magnetic field lines entangle and snap, releasing large amounts of energy. Scientists are not sure exactly what causes these eruptions, but they are believed to be caused by a strong magnetic field. In fact, these explosions can be observed on many stars, including Venus and Jupiter.
Space weather is the unpredictable weather in our solar system, and auroras are an example of this. Solar flares, which are massive explosions on the sun's surface, emit charged particles into space, triggering auroras as they reach Earth. Coronal mass ejections, or CMEs, are another type of solar activity that generates intense aurora displays. These clouds of hot plasma travel to Earth at a rate of two million miles per hour and interact with the Earth's magnetic field.
Solar winds on the Sun are continuous flows of protons and electrons in a plasma state. These winds are accompanied by an embedded magnetic field, which affects the Earth. Solar wind speed and density are crucial for space weather forecasts. As solar winds move around the Earth, they can trigger geomagnetic storms or calm space weather. The intensity of the solar wind is strongly affected by the density and speed of the solar magnetic field.
The equatorial zones of the Sun rotate faster than the poles. Therefore, it would take 26 days to travel around the Sun if you stood on the solar equator. In contrast, it would take over 32 days to travel around the Sun if you stood close to the poles. This differential rotation is known as helioseismology. In addition, the Sun has a polar region.
The temperature of a naked man in still air is approximately 25 degrees Celsius (77 degrees Fahrenheit) and lower in the convective zone of the Sun, where the heat is concentrated. This area is also used in the making of clothes, including tanning and coloring. The temperature of the convective zone is approximately five to eight thousand degrees, and it extends from just below the photosphere and surrounds the Core and Radiative zone. The difference between the temperature of the photosphere and the convective zone is a result of thermal radiation.