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The Sun is composed primarily of the chemical elements hydrogen and helium; they account for 74.9% and 23.8%, respectively, of the mass of the Sun in the photosphere.All heavier elements, colloquially called metals in stellar 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.
Together, the new images showcase the sun’s varied and complex layers. ... or photosphere, to date. Nearly all radiation from the sun originates from the photosphere, with sizzling temperatures ...
The spectrum of sunlight has approximately the spectrum of a black-body radiating at 5,772 K (9,930 °F), [12] interspersed with atomic absorption lines from the tenuous layers above the photosphere. The photosphere has a particle density of ~10 23 m −3 (about 0.37% of the particle number per volume of Earth's atmosphere at sea level). The ...
The expanding photosphere method (EPM) is a method used to measure distances to Type II supernovae. It was developed by Robert Kirshner and John Kwan in 1974, based on the Baade–Wesselink method (1926). [1] [2] EPM is a geometrical method that compares a supernova's angular size to its physical size determined from spectroscopic measurements. [3]
The photosphere, which is the atmosphere's lowest and coolest layer, is normally its only visible part. [1] Light escaping from the surface of the star stems from this region and passes through the higher layers. The Sun's photosphere has a temperature in the 5,770–5,780 K (5,500–5,510 °C; 9,930–9,940 °F) range.
A radiative zone is a layer of a star's interior where energy is primarily transported toward the exterior by means of radiative diffusion and thermal conduction, rather than by convection. [1] Energy travels through the radiative zone in the form of electromagnetic radiation as photons .
The Sun is a rotating sphere of plasma at the center of the Solar System. It lacks a solid or liquid surface, so the interface separating its interior and its exterior is usually defined as the boundary where plasma becomes opaque to visible light, the photosphere.
The photosphere denotes those solar or stellar surface layers from which optical radiation escapes. These stellar outer layers can be modeled by different computer programs. Often, calculated models are used, together with other programs, to calculate synthetic spectra for stars. For example, in varying the assumed abundance of a chemical ...