Through the overlying layers of the Sun and, with some effort, can be detected here onĮarth.
Produce elementary particles called neutrinos. In this process of fusing hydrogen to form helium, the nuclear reactions To produce a normal helium-4 nucleus with the release of two protons. With the deuterium to produce a helium-3 nucleus and a gamma ray. To produce deuterium, a positron, and a neutrino. Through a three step process called the proton-proton or pp chain.
In stars like the Sun the nuclear burning takes place That point the temperature is only half its central value and the density drops to about Of the core (about 25% of the distance to the surface or 175,000 km from the center). The nuclear burning is almost completely shut off beyond the outer edge Both the temperature and the density decrease as one moves outward from theĬenter of the Sun. (27,000,000° F) and the density is about 150 g/cm³ (approximately 10 times the density of gold, 19.3 g/cm³ or lead, 11.3 g/cm³). The temperature at the very center of the Sun is about 15,000,000° C Probability of overcoming the repulsive electrical force between these two positivelyĬharged particles. The individual hydrogen nuclei must collide with enough energy to give a reasonable These reactions are highly sensitive to temperature and density. These reactions release the energy that ultimately leaves the The Sun's core is the central region where nuclear reactions consume Layer (the "tachocline") between the radiative zone and the convection Energy is generated in the core, the innermostīy radiation (mostly gamma-rays and x-rays) through the radiative zone andīy convective fluid flows (boiling motion) through the convection zone, the The solar interior is separated into four Marshall Grazing Incidence X-ray Spectrometer (MaGIXS) Chromospheric Lyman-Alpha Spectro Polarimeter (CLASP)
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