Sun | Wikipedia audio article
Channel: wikipedia tts
Date: 15/12/2018

This is an audio version of the Wikipedia Article:
Sun


00:02:41 1 Name and etymology
00:04:03 1.1 Religious aspects
00:06:50 2 Characteristics
00:09:41 3 Sunlight
00:11:49 4 Composition
00:14:37 4.1 Singly ionized iron-group elements
00:15:21 4.2 Isotopic composition
00:16:01 5 Structure and energy production
00:17:46 5.1 Core
00:20:54 5.2 Radiative zone
00:21:48 5.3 Tachocline
00:22:26 5.4 Convective zone
00:24:04 5.5 Photosphere
00:25:51 5.6 Atmosphere
00:29:39 5.7 Photons and neutrinos
00:31:20 6 Magnetism and activity
00:31:29 6.1 Magnetic field
00:35:43 6.2 Variation in activity
00:36:44 6.3 Long-term change
00:37:44 7 Life phases
00:38:13 7.1 Formation
00:39:50 7.2 Main sequence
00:41:12 7.3 After core hydrogen exhaustion
00:45:04 8 Motion and location
00:46:18 8.1 Orbit in Milky Way
00:50:35 9 Theoretical problems
00:57:48 9.1 Coronal heating problem
00:57:57 9.2 Faint young Sun problem
00:59:18 10 History of observation
01:00:36 10.1 Early understanding
01:00:55 10.2 Development of scientific understanding
01:02:48 10.3 Solar space missions
01:07:25 11 Observation and effects
01:08:19 12 Planetary system
01:13:14 13 See also
01:17:44 14 Notes
01:18:16 15 References



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SUMMARY
=======
The Sun is the star at the center of the Solar System. It is a nearly perfect sphere of hot plasma, with internal convective motion that generates a magnetic field via a dynamo process. It is by far the most important source of energy for life on Earth. Its diameter is about 1.39 million kilometers, or 109 times that of Earth, and its mass is about 330,000 times that of Earth. It accounts for about 99.86% of the total mass of the Solar System.
About three quarters of the Sun's mass consists of hydrogen (~73%); the rest is mostly helium (~25%), with much smaller quantities of heavier elements, including oxygen, carbon, neon, and iron.The Sun is a G-type main-sequence star (G2V) based on its spectral class. As such, it is informally and not completely accurately referred to as a yellow dwarf (its light is closer to white than yellow). It formed approximately 4.6 billion years ago from the gravitational collapse of matter within a region of a large molecular cloud. Most of this matter gathered in the center, whereas the rest flattened into an orbiting disk that became the Solar System. The central mass became so hot and dense that it eventually initiated nuclear fusion in its core. It is thought that almost all stars form by this process.
The Sun is roughly middle-aged; it has not changed dramatically for more than four billion years, and will remain fairly stable for more than another five billion years. It currently fuses about 600 million tons of hydrogen into helium every second, converting 4 million tons of matter into energy every second as a result. This energy, which can take between 10,000 and 170,000 years to escape from its core, is the source of the Sun's light and heat. In about 5 billion years, when hydrogen fusion in its core has diminished to the point at which the Sun is no longer in hydrostatic equilibrium, its core will undergo a marked increase in density and temperature while its outer layers expand to eventually become a red giant. It is calculated that the Sun will become sufficiently large to engulf the current orbits of Mercury and Venus, and render Earth uninhabitable. After this, it will shed its outer layers and become a dense type of cooling star known as a white dwarf, and no longer produce energy by fusion, but still glow and give off heat from its previous fusion.
The enormous effect of the Sun on Earth has been recognized since prehistoric times, and the Sun has been regarded by some cultures as a deity. The synodic rotation of Earth and its orbit around the Sun are the basis of solar calendars, one of which is the predominant calendar in use today.