Kelvin–Helmholtz mechanism
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The Kelvin–Helmholtz mechanism is an
astronomical Astronomy () is a natural science that studies celestial objects and phenomena. It uses mathematics, physics, and chemistry in order to explain their origin and evolution. Objects of interest include planets, moons, stars, nebulae, galaxi ...
process that occurs when the surface of a star or a
planet A planet is a large, rounded astronomical body that is neither a star nor its remnant. The best available theory of planet formation is the nebular hypothesis, which posits that an interstellar cloud collapses out of a nebula to create a you ...
cools. The cooling causes the internal pressure to drop, and the star or planet shrinks as a result. This compression, in turn, heats the core of the star/planet. This mechanism is evident on
Jupiter Jupiter is the fifth planet from the Sun and the largest in the Solar System. It is a gas giant with a mass more than two and a half times that of all the other planets in the Solar System combined, but slightly less than one-thousandth t ...
and Saturn and on
brown dwarf Brown dwarfs (also called failed stars) are substellar objects that are not massive enough to sustain nuclear fusion of ordinary hydrogen ( 1H) into helium in their cores, unlike a main-sequence star. Instead, they have a mass between the most ...
s whose central temperatures are not high enough to undergo hydrogen fusion. It is estimated that Jupiter radiates more energy through this mechanism than it receives from the Sun, but Saturn might not. Jupiter has been estimated to shrink at a rate of approximately 1 mm/year by this process, corresponding to an internal flux of 7.485 W/m2. The mechanism was originally proposed by
Kelvin The kelvin, symbol K, is the primary unit of temperature in the International System of Units (SI), used alongside its prefixed forms and the degree Celsius. It is named after the Belfast-born and University of Glasgow-based engineer and phy ...
and Helmholtz in the late nineteenth century to explain the source of energy of the
Sun The Sun is the star at the center of the Solar System. It is a nearly perfect ball of hot plasma, heated to incandescence by nuclear fusion reactions in its core. The Sun radiates this energy mainly as light, ultraviolet, and infrared radi ...
. By the mid-nineteenth century, conservation of energy had been accepted, and one consequence of this law of physics is that the Sun must have some energy source to continue to shine. Because nuclear reactions were unknown, the main candidate for the source of solar energy was gravitational contraction. However, it soon was recognized by Sir Arthur Eddington and others that the total amount of energy available through this mechanism only allowed the Sun to shine for millions of years rather than the billions of years that the geological and biological evidence suggested for the age of the Earth. (Kelvin himself had argued that the Earth was millions, not billions, of years old.) The true source of the Sun's energy remained uncertain until the 1930s, when it was shown by
Hans Bethe Hans Albrecht Bethe (; July 2, 1906 – March 6, 2005) was a German-American theoretical physicist who made major contributions to nuclear physics, astrophysics, quantum electrodynamics, and solid-state physics, and who won the 1967 Nobel ...
to be
nuclear fusion Nuclear fusion is a reaction in which two or more atomic nuclei are combined to form one or more different atomic nuclei and subatomic particles ( neutrons or protons). The difference in mass between the reactants and products is manife ...
.


Power generated by a Kelvin–Helmholtz contraction

It was theorised that the
gravitational potential energy Gravitational energy or gravitational potential energy is the potential energy a massive object has in relation to another massive object due to gravity. It is the potential energy associated with the gravitational field, which is released (conver ...
from the contraction of the Sun could be its source of power. To calculate the total amount of energy that would be released by the Sun in such a mechanism (assuming uniform
density Density (volumetric mass density or specific mass) is the substance's mass per unit of volume. The symbol most often used for density is ''ρ'' (the lower case Greek letter rho), although the Latin letter ''D'' can also be used. Mathematical ...
), it was approximated to a perfect sphere made up of concentric shells. The gravitational potential energy could then be found as the integral over all the shells from the centre to its outer radius. Gravitational potential energy from Newtonian mechanics is defined as: :U = -\frac, where ''G'' is the gravitational constant, and the two masses in this case are that of the thin shells of width ''dr'', and the contained mass within radius ''r'' as one integrates between zero and the radius of the total sphere. This gives: :U = -G\int_0^R \frac\, dr, where ''R'' is the outer radius of the sphere, and ''m''(''r'') is the mass contained within the radius ''r''. Changing ''m''(''r'') into a product of volume and density to satisfy the integral, :U = -G\int_0^R \frac\, dr = -\fracG \pi^2 \rho^2 R^5. Recasting in terms of the mass of the sphere gives the total gravitational potential energy as :U = -\frac. According to the
Virial Theorem In mechanics, the virial theorem provides a general equation that relates the average over time of the total kinetic energy of a stable system of discrete particles, bound by potential forces, with that of the total potential energy of the system. ...
, the total energy for gravitationally bound systems in equilibrium is one half of the time-averaged potential energy, :U_r = \frac = \frac. While uniform density is not correct, one can get a rough order of magnitude estimate of the expected age of our star by inserting known values for the
mass Mass is an intrinsic property of a body. It was traditionally believed to be related to the quantity of matter in a physical body, until the discovery of the atom and particle physics. It was found that different atoms and different eleme ...
and radius of the Sun, and then dividing by the known
luminosity of the Sun The solar luminosity (), is a unit of radiant flux ( power emitted in the form of photons) conventionally used by astronomers to measure the luminosity of stars, galaxies and other celestial objects in terms of the output of the Sun. One nominal ...
(note that this will involve another approximation, as the power output of the Sun has not always been constant): :\frac \approx \frac = 2.874\times10^~\mathrm \, \approx 8\,900\,000~\text, where L_\odot is the luminosity of the Sun. While giving enough power for considerably longer than many other physical methods, such as chemical energy, this value was clearly still not long enough due to geological and biological evidence that the Earth was billions of years old. It was eventually discovered that
thermonuclear Thermonuclear fusion is the process of atomic nuclei combining or “fusing” using high temperatures to drive them close enough together for this to become possible. There are two forms of thermonuclear fusion: ''uncontrolled'', in which the re ...
energy was responsible for the power output and long lifetimes of stars. The flux of internal heat for Jupiter is given by the derivative according to the time of the total energy :\frac = \frac \frac = -1.46 \times 10^~\text~\times\frac~\text. With a shrinking of -1\mathrm\frac = -0.001\mathrm\frac = -3.17\times 10^~\mathrm\frac, one gets :\frac = 4.63\times 10^~\text, dividing by the whole area of Jupiter, i.e. S = 6.14\times 10^~\mathrm, one gets :\frac\frac = 7.5~\mathrm\frac. Of course, one usually calculates this equation in the other direction: the experimental figure of the specific flux of internal heat, 7.485 W/m2, was given from the direct measures made on the spot by the
Cassini probe Cassini may refer to: People * Cassini (surname) * Oleg Cassini (1913-2006), American fashion designer :Cassini family: * Giovanni Domenico Cassini (1625–1712), Italian mathematician, astronomer, engineer, and astrologer * Jacques Cassini (16 ...
during its flyby on 30 December 2000 and one gets the amount of the shrinking, ~1 mm/year, a minute figure below every measurement.


References

{{DEFAULTSORT:Kelvin-Helmholtz Mechanism Astrophysics Stellar evolution Effects of gravitation Mechanism William Thomson, 1st Baron Kelvin