Starship Asterisk*

Orca wrote:Globular clusters always fascinated me as a kid; there are so many beautiful images of them. What really got me thinking lately was the structure of globular clusters. You'd think that a close proximity of a large group of stars ought to collapse inward given enough time.

Orca wrote:
Globular clusters always fascinated me as a kid; there are so many beautiful images of them. What really got me thinking lately was the structure of globular clusters. You'd think that a close proximity of a large group of stars ought to collapse inward given enough time. Yet globular clusters, as old as they are, persist. So, while the overall structure is stable, the individual stars are all moving - imagine how complex the interactions must be between 10,000 individual stars moving around one another!

http://en.wikipedia.org/wiki/Virial_theorem wrote:
<<The word "virial" derives from vis, the Latin word for "force" or "energy", and was given its technical definition by Clausius in 1870. In mechanics, the virial theorem provides a general equation relating the average over time of the total kinetic energy, , of a stable system consisting of N particles, bound by potential forces, with that of the total potential energy, , where angle brackets represent the average over time of the enclosed quantity.

Mathematically, the theorem states:

where F_k represents the force on the kth particle, which is located at position r_k.

If the force between any two particles of the system results from a potential energy V(r) = αrⁿ that is proportional to some power n of the inter-particle distance r, the virial theorem adopts a simple form: . Thus, twice the average total kinetic energy equals n times the average total potential energy . Whereas V(r) represents the potential energy between two particles, V_TOT represents the total potential energy of the system, i.e., the sum of the potential energy V(r) over all pairs of particles in the system. A common example of such a system is a star held together by its own gravity, where n equals −1.

Although the virial theorem depends on averaging the total kinetic and potential energies, the presentation here postpones the averaging to the last step. The significance of the virial theorem is that it allows the average total kinetic energy to be calculated even for very complicated systems that defy an exact solution, such as those considered in statistical mechanics; this average total kinetic energy is related to the temperature of the system by the equipartition theorem. However, the virial theorem does not depend on the notion of temperature and holds even for systems that are not in thermal equilibrium. The virial theorem has been generalized in various ways, most notably to a tensor form.

History of the virial theorem

In 1870, Rudolf Clausius delivered the lecture "On a Mechanical Theorem Applicable to Heat" to the Association for Natural and Medical Sciences of the Lower Rhine, following a 20 year study of thermodynamics. The lecture stated that the mean vis viva of the system is equal to its virial, or that the average kinetic energy is equal to 1/2 the average potential energy. The virial theorem can be obtained directly from Lagrange's Identity as applied in classical gravitational dynamics, the original form of which was included in his "Essay on the Problem of Three Bodies" published in 1772. Karl Jacobi's generalization of the identity to n bodies and to the present form of Laplace's identity closely resembles the classical virial theorem. However, the interpretations leading to the development of the equations were very different, since at the time of development, statistical dynamics had not yet unified the separate studies of thermodynamics and classical dynamics. The theorem was later utilized, popularized, generalized and further developed by persons such as James Clerk Maxwell, Lord Rayleigh, Henri Poincaré, Subrahmanyan Chandrasekhar, Enrico Fermi, Paul Ledoux and Eugene Parker. Fritz Zwicky was the first to use the virial theorem to deduce the existence of unseen matter, which is now called dark matter. As another example of its many applications, the virial theorem has been used to derive the Chandrasekhar limit for the stability of white dwarf stars. Lord Rayleigh published a generalization of the virial theorem in 1903. Although derived for classical mechanics, the virial theorem also holds for quantum mechanics.
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For power-law forces with an exponent n, the general equation holds



For gravitational attraction, n equals −1 and the average kinetic energy equals half of the average negative potential energy



This general result is useful for complex gravitating systems such as solar systems or galaxies.

A simple application of the virial theorem concerns galaxy clusters. If a region of space is unusually full of galaxies, it is safe to assume that they have been together for a long time, and the virial theorem can be applied. Doppler measurements give lower bounds for their relative velocities, and the virial theorem gives a lower bound for the total mass of the cluster, including any dark matter.

The averaging need not be taken over time; an ensemble average can also be taken, with equivalent results.>>

neufer wrote: (Virile, a. [L. virilis, fr. vir a man; akin to AS. wer.] Having the nature, properties, or qualities, of an adult man; characteristic of developed manhood; hence, masterful; forceful; specifically, capable of begetting; --

owlice wrote:

neufer wrote: (Virile, a. [L. virilis, fr. vir a man; akin to AS. wer.] Having the nature, properties, or qualities, of an adult man; characteristic of developed manhood; hence, masterful; forceful; specifically, capable of begetting; --

I took one course in virology in college (really hard, really interesting, and almost as cool as hematology); you would not believe (or maybe you would) how many people thought I was making a joke involving manly men when I mentioned it! Telling them I worked in a diagnostic lab doing, among other things, sperm analyses did not help matters. The comic potential completely escaped me back then.

Chris Peterson wrote:

Orca wrote:Globular clusters always fascinated me as a kid; there are so many beautiful images of them. What really got me thinking lately was the structure of globular clusters. You'd think that a close proximity of a large group of stars ought to collapse inward given enough time.

Why would you think this? Should stellar systems collapse for the same reason? (That is, should all the planets end up in the Sun?) For the system to collapse, you'd need a mechanism that could remove an awful lot of energy from the system.

In fact, what actually happens is that globulars slowly fall apart, and evaporate away- just the opposite of collapsing.

Chris Peterson wrote:

Orca wrote:
Globular clusters always fascinated me as a kid; there are so many beautiful images of them. What really got me thinking lately was the structure of globular clusters. You'd think that a close proximity of a large group of stars ought to collapse inward given enough time.

Why would you think this? Should stellar systems collapse for the same reason? (That is, should all the planets end up in the Sun?) For the system to collapse, you'd need a mechanism that could remove an awful lot of energy from the system.

In fact, what actually happens is that globulars slowly fall apart, and evaporate away- just the opposite of collapsing.

neufer wrote:In fact, what actually happens is that globulars slowly evaporate while simultaneously
condensing into a smaller cluster full of blue stragglers and black holes.

Orca wrote:We know globular clusters are very old, so the process of evaporation must take a while. Have astronomers speculated on possible variables that might affect the length of time it takes for a cluster to evaporate? Overall mass? Relative velocities of stars within the cluster?

Orca wrote:We know globular clusters are very old, so the process of evaporation must take a while. Have astronomers speculated on possible variables that might affect the length of time it takes for a cluster to evaporate? Overall mass? Relative velocities of stars within the cluster?