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Comparing Earth, Sun and Jupiter
Comparing Earth, Sun and Jupiter

...  The density, pressure and temperature are related by the equation of state, which can usually be approximated as the ideal gas law. ...
Review2
Review2

... a. Stability of the Sun: balance between gravity and pressure (so-called hydrostatic equilibrium – meaning static water, but the sun is not made of water!) b. Zones of the Sun: energy production (at the core) and transport (from the core out of the Sun). c. Characteristics of the outer layers – phot ...
The Sun
The Sun

... The center of the sun Very, very hot At the core, gravity pulls all of the mass inward and creates an intense pressure. The pressure is high enough to force atoms of hydrogen to come together in nuclear fusion reactions -something we try to mirror here on Earth. ...
The Sun
The Sun

... • Class G • Color Yellow • Surface Temperature 5,000 – 6,000 ºC • Elements hydrogen and helium • Greek word for Sun is Helios ...
AST301.Ch16.Sun
AST301.Ch16.Sun

... One way out: maybe neutrinos do have mass (unlike photons), in which case they can spontaneously transform into other types of neutrinos, along their path from the earth to the sun, which would not be detected by the experiments. These possible transormation among neutrinos are called “neutrino osc ...
The Sun - University of Redlands
The Sun - University of Redlands

... At and above the corona: Gas is very hot Very energetic Like steam above our boiling pot of water, the gas ‘evaporates’. • Wind passes out through Coronal Holes • Solar Wind carries away a million tons of Sun’s mass each second! • Only 0.1% of total Sun’s mass in last 4.6 billion years. ...
Astrophysics
Astrophysics

... 3.9 x 1026 watts . ...
Lecture13 - University of Waterloo
Lecture13 - University of Waterloo

... neutrinos (by a factor 2-3) than were expected from the PP-chain reactions. This problem existed for about 30 years. The solution to the problem was suggested by results from the Super-Kamiokande detector in Japan ...
Insides3
Insides3

... & fuse – form heavier particle. ...
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Standard solar model

The standard solar model (SSM) is a mathematical treatment of the Sun as a spherical ball of gas (in varying states of ionisation, with the hydrogen in the deep interior being a completely ionised plasma). This model, technically the spherically symmetric quasi-static model of a star, has stellar structure described by several differential equations derived from basic physical principles. The model is constrained by boundary conditions, namely the luminosity, radius, age and composition of the Sun, which are well determined. The age of the Sun cannot be measured directly; one way to estimate it is from the age of the oldest meteorites, and models of the evolution of the Solar System. The composition in the photosphere of the modern-day Sun, by mass, is 74.9% hydrogen and 23.8% helium. All heavier elements, called metals in astronomy, account for less than 2 percent of the mass. The SSM is used to test the validity of stellar evolution theory. In fact, the only way to determine the two free parameters of the stellar evolution model, the helium abundance and the mixing length parameter (used to model convection in the Sun), are to adjust the SSM to ""fit"" the observed Sun.
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