![]() ![]() The Sun by the Atmospheric Imaging Assembly of NASA's Solar Dynamics Observatory - 20100819. Solar Lower Atmosphere and Magnetism (MPS)Ĭore Radiation zone Tachocline Convection zone "The Sun's Vital Statistics".Īnimated explanation of the Photosphere (University of South Wales).Īnimated explanation of the temperature of the Photosphere (University of South Wales). "SP-402 A New Sun: The Solar Results From Skylab". Addison-Wesley.Īs of 2004, although white dwarfs are believed to crystallize from the middle out, none have fully solidified yet and only neutron stars are believed to have a solid, albeit unstable, crust The temperature of this region is between 4,500 and 6,000 Kelvin. Within this zone, we see sunspots, solar flares, granules and convection cells. Photosphere (Sphere of light) This is the surface layer of. This part of the Sun is very thin (just 100 km or 62 miles thick) compared to other regions of the Sun, such as the corona and chromosphere. Other "surface features" on the photosphere are solar flares and sunspots.Ĭarroll, Bradley W. Light and heat move through these regions of the Sun, temperatures range from 2,000,000K to 6,000K. It is found that the ratio of minimum temperature to effective temperature is approximately 0.77 for Arcturus, Procyon, and the sun, and that mass tends to increase at the temperature minimum with. ![]() The Sun's visible atmosphere has other layers above the photosphere: the 2,000 kilometer-deep chromosphere (typically observed by filtered light, for example H-alpha) lies just between the photosphere and the much hotter but more tenuous corona. These details are too fine to be seen when observing other stars from earth. Instead of being about 5700 degrees kelvin like the rest of the photosphere, the temperature of a. Other magnetically-related phenomena include sunspots and solar faculae dispersed between the granules. But as Fisher points out, sunspots are actually quite hot. Grouping the typical granules are super granules up to 30,000 kilometers in diameter with lifespans of up to 24 hours and flow speeds of about 500 meter per second, carrying magnetic field bundles to the edges of the cells. Each granule has a lifespan of only about twenty minutes, resulting in a continually shifting "boiling" pattern. The Sun's photosphere is around 100 kilometers thick, and is composed of convection cells called granules-cells of plasma each approximately 1000 kilometers in diameter with hot rising plasma in the center and cooler plasma falling in the narrow spaces between them, flowing at velocities of 7 kilometer per second. Other stars may have hotter or cooler photospheres. The Sun's photosphere has a temperature between 4,500 and 6,000 K (4,230 and 5,730 ☌) (with an effective temperature of 5,777 K (5,504 ☌)) and a density of about 3×10−4 kg/m3 increasing with depth into the sun. See here for meanings of extra lines in the graph. Solar atmosphere: temperature and density. All heavier elements, called metals in astronomy, account for less than 2% of the mass, with oxygen (roughly 1% of the Sun's mass), carbon (0.3%), neon (0.2%), and iron (0.2%) being the most abundant. The Sun is composed primarily of the chemical elements hydrogen and helium they account for 74.9% and 23.8% of the mass of the Sun in the photosphere, respectively. Therefore, the photosphere is typically used to describe the Sun's or another star's visual surface. Stars, except neutron stars, have no solid or liquid surface. The surface of a star is defined to have a temperature given by the effective temperature in the Stefan–Boltzmann law. It extends into a star's surface until the plasma becomes opaque, equivalent to an optical depth of approximately 2⁄3, or equivalently, a depth from which 50% of light will escape without being scattered.Ī photosphere is the deepest region of a luminous object, usually a star, that is transparent to photons of certain wavelengths. The term itself is derived from Ancient Greek roots, φῶς, φωτός/phos, photos meaning "light" and σφαῖρα/sphaira meaning "sphere", in reference to it being a spherical surface that is perceived to emit light. This layer extends far into space and is shaped by the Sun's magnetic field, is visible only during eclipses or with special equipment.The photosphere is a star's outer shell from which light is radiated. The eighth and outer layer of the Sun gets extremely hot, measuring 1,800,000☏ more. The layer between the hot corona and cooler chromosphere A thin, reddish layer, the chromosphere is seen only during eclipses or with special solar-viewing equipment. The sixth layer is where the temperature begins to rise again. The fifth layer is the visible surface where sunspots appear. The fourth layer is a zone of boiling, bubbling plasma that transfers energy outward through a process called convection. The second layer becomes cooler and is where photon particles carry energy in all directions through a process called radiation.Ī thin third layer, the tachocline acts as a border between two differently rotating zones. The hottest part of the Sun is the core, at 28,080,000☏, on average. ![]()
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