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In stellar physics, the Jeans instability causes the collapse of interstellar gas clouds and subsequent star formation, named after James Jeans. It occurs when the internal gas pressure is not strong enough to prevent gravitational collapse of a region filled with matter. For stability, the cloud must be in hydrostatic equilibrium, which in case of a spherical cloud translates to:

\( {\displaystyle {\frac {dp}{dr}}=-{\frac {G\rho (r)M_{\text{enc}}(r)}{r^{2}}}}, \)
where \( {\textstyle M_{\text{enc}}(r)} \) is the enclosed mass, \( {\textstyle p} \) is the pressure, \( {\textstyle \rho (r)} \) is the density of the gas (at radius \( {\textstyle r}) \), \( {\textstyle G} \) is the gravitational constant, and \( {\textstyle r} \) is the radius. The equilibrium is stable if small perturbations are damped and unstable if they are amplified. In general, the cloud is unstable if it is either very massive at a given temperature or very cool at a given mass; under these circumstances, the gas pressure cannot overcome gravity, and the cloud will collapse.

Jeans mass

The Jeans mass is named after the British physicist Sir James Jeans, who considered the process of gravitational collapse within a gaseous cloud. He was able to show that, under appropriate conditions, a cloud, or part of one, would become unstable and begin to collapse when it lacked sufficient gaseous pressure support to balance the force of gravity. The cloud is stable for sufficiently small mass (at a given temperature and radius), but once this critical mass is exceeded, it will begin a process of runaway contraction until some other force can impede the collapse. He derived a formula for calculating this critical mass as a function of its density and temperature. The greater the mass of the cloud, the smaller its size, and the colder its temperature, the less stable it will be against gravitational collapse.

The approximate value of the Jeans mass may be derived through a simple physical argument. One begins with a spherical gaseous region of radius \( {\textstyle R} \) , mass \( {\textstyle M} \) , and with a gaseous sound speed c s {\textstyle c_{s}} {\textstyle c_{s}}. The gas is compressed slightly and it takes a time

\( {\displaystyle t_{\text{sound}}={\frac {R}{c_{s}}}\approx 0.5{\mbox{ Myr}}\cdot {\frac {R}{0.1{\mbox{ pc}}}}\cdot \left({\frac {c_{s}}{0.2{\mbox{ km s}}^{-1}}}\right)^{-1}} \)

for sound waves to cross the region and attempt to push back and re-establish the system in pressure balance. At the same time, gravity will attempt to contract the system even further, and will do so on a free-fall time,

\( {\displaystyle t_{\rm {ff}}={\frac {1}{(G\rho )^{\frac {1}{2}}}}\approx 2{\mbox{ Myr}}\cdot \left({\frac {n}{10^{3}{\mbox{ cm}}^{-3}}}\right)^{-{\frac {1}{2}}}} \)

where \( {\textstyle G} \) is the universal gravitational constant, \( {\textstyle \rho } \) is the gas density within the region, and \( {\textstyle n=\rho /\mu } \) is the gas number density for mean mass per particle (μ = 3.9×10−24 g is appropriate for molecular hydrogen with 20% helium by number). When the sound-crossing time is less than the free-fall time, pressure forces temporarily overcome gravity, and the system returns to a stable equilibrium. However, when the free-fall time is less than the sound-crossing time, gravity overcomes pressure forces, and the region undergoes gravitational collapse. The condition for gravitational collapse is therefore:

\( {\displaystyle t_{\rm {ff}}<t_{\text{sound}}.} \)

The resultant Jeans length \( {\textstyle \lambda _{\text{J}}} \) is approximately:

\( {\displaystyle \lambda _{\text{J}}={\frac {c_{s}}{(G\rho )^{\frac {1}{2}}}}\approx 0.4{\mbox{ pc}}\cdot {\frac {c_{s}}{0.2{\mbox{ km s}}^{-1}}}\cdot \left({\frac {n}{10^{3}{\mbox{ cm}}^{-3}}}\right)^{-{\frac {1}{2}}}.} \)

This length scale is known as the Jeans length. All scales larger than the Jeans length are unstable to gravitational collapse, whereas smaller scales are stable. The Jeans mass \( {\textstyle M_{\text{J}}} \) is just the mass contained in a sphere of radius \( {\textstyle R_{\text{J}}} \) ( \( {\textstyle R_{\text{J}}={\frac {1}{2}}\lambda _{\text{J}}} \) is half the Jeans length):

\( {\displaystyle M_{\text{J}}={\frac {4\pi }{3}}\rho R_{\text{J}}^{3}={\frac {\pi }{6}}\cdot {\frac {c_{s}^{3}}{G^{\frac {3}{2}}\rho ^{\frac {1}{2}}}}\approx 2{\mbox{ M}}_{\odot }\cdot \left({\frac {c_{s}}{0.2{\mbox{ km s}}^{-1}}}\right)^{3}\left({\frac {n}{10^{3}{\mbox{ cm}}^{-3}}}\right)^{-{\frac {1}{2}}}.} \)

It was later pointed out by other astrophysicists that in fact, the original analysis used by Jeans was flawed, for the following reason. In his formal analysis, Jeans assumed that the collapsing region of the cloud was surrounded by an infinite, static medium. In fact, because all scales greater than the Jeans length are also unstable to collapse, any initially static medium surrounding a collapsing region will also be collapsing. As a result, the growth rate of the gravitational instability relative to the density of the collapsing background is slower than that predicted by Jeans' original analysis. This flaw has come to be known as the "Jeans swindle".

The Jeans instability likely determines when star formation occurs in molecular clouds.

An alternative, arguably even simpler, derivation can be found using energy considerations. In the interstellar cloud, two opposing forces are at work. The gas pressure, caused by the thermal movement of the atoms or molecules comprising the cloud, tries to make the cloud expand, whereas gravitation tries to make the cloud collapse. The Jeans mass is the critical mass where both forces are in equilibrium with each other. In the following derivation numerical constants (such as π) and constants of nature (such as the gravitational constant) will be ignored. They will be reintroduced in the end result.

Consider a homogenous spherical gas cloud with radius R. In order to compress this sphere to a radius R – dR, work must be done against the gas pressure. During the compression, gravitational energy is released. When this energy equals the amount of work to be done on the gas, the critical mass is attained. Let M be the mass of the cloud, T the (absolute) temperature, n the particle density, and p the gas pressure. The work to be done equals p dV. Using the ideal gas law, according to which p = nT, one arrives at the following expression for the work:

\( {\displaystyle dW=nTR^{2}dR} \)

The gravitational potential energy of a sphere with mass M and radius R is, apart from constants, given by the following expression:

\( {\displaystyle U={\frac {M^{2}}{R}}} \)

The amount of energy released when the sphere contracts from radius R to radius R – dR is obtained by differentiation this expression to R, so

\( {\displaystyle dU={\frac {M^{2}}{R^{2}}}dR} \)

The critical mass is attained as soon as the released gravitational energy is equal to the work done on the gas:

\( {\displaystyle {\frac {M^{2}}{R^{2}}}=nTR^{2}} \)

Next, the radius R must be expressed in terms of the particle density n and the mass M. This can be done using the relation

\( {\displaystyle M=nR^{3}} \)

A little algebra leads to the following expression for the critical mass.

\( {\displaystyle M_{\text{J}}=\left({\frac {T^{3}}{n}}\right)^{\frac {1}{2}}} \)

If during the derivation all constants are taken along, the resulting expression is

\( {\displaystyle M_{\text{J}}=\left({\frac {375k^{3}}{4\pi m^{4}G^{3}}}\right)^{\frac {1}{2}}\left({\frac {T^{3}}{n}}\right)^{\frac {1}{2}}} \)

where k is Boltzmann's constant, G the gravitational constant, and m the mass of a particle comprising the gas. Assuming the cloud to consist of atomic hydrogen, the prefactor can be calculated. If we take the solar mass as the unit of mass, the result is

\( {\displaystyle M_{\text{J}}=3\times 10^{4}\left({\frac {T^{3}}{n}}\right)^{\frac {1}{2}}} \)

Jeans' length

Jeans' length is the critical radius of a cloud (typically a cloud of interstellar molecular gas and dust) where thermal energy, which causes the cloud to expand, is counteracted by gravity, which causes the cloud to collapse. It is named after the British astronomer Sir James Jeans, who concerned himself with the stability of spherical nebulae in the early 1900s.[1]

The formula for Jeans length is:

\( {\displaystyle \lambda _{\text{J}}=\left({\frac {15k_{\text{B}}T}{4\pi Gm_{p}\mu \rho }}\right)^{\frac {1}{2}},} \)

where \( {\textstyle k_{\text{B}}} \) is Boltzmann's constant, \( {\textstyle T} \) is the temperature of the cloud, \( {\textstyle \mu } \) is the mass per particle in the cloud,\( {\textstyle G} \) is the gravitational constant, \( {\textstyle m_{p},} \) is the mass of a proton in kg, and \( {\textstyle \rho } \) is the cloud's mass density (i.e. the cloud's mass divided by the cloud's volume).[2]

Perhaps the easiest way to conceptualize Jeans' length is in terms of a close approximation, in which we discard the factors \( {\textstyle 15} \) and \( {\textstyle 4\pi } \) and in which we rephrase \( {\textstyle \rho } \) as \( {\textstyle {\frac {M}{r^{3}}}} \) . The formula for Jeans' length then becomes:

\( {\displaystyle \lambda _{\text{J}}\approx \left({\frac {k_{\text{B}}Tr^{3}}{GM\mu }}\right)^{\frac {1}{2}}.} \)

where r {\textstyle r} {\textstyle r} is the radius of the cloud.

It follows immediately that \( {\textstyle \lambda _{\text{J}}=r} \) when \( {\textstyle k_{\text{B}}T={\frac {GM\mu }{r}}} \); i.e., the cloud's radius is the Jeans' length when thermal energy per particle equals gravitational work per particle. At this critical length the cloud neither expands nor contracts. It is only when thermal energy is not equal to gravitational work that the cloud either expands and cools or contracts and warms, a process that continues until equilibrium is reached.
Jeans' length as oscillation wavelength

The Jeans' length is the oscillation wavelength (respectively, Jeans' wavenumber, \( {\textstyle k_{\text{J}}}) \) below which stable oscillations rather than gravitational collapse will occur.

\( {\displaystyle \lambda _{\text{J}}={\frac {2\pi }{k_{\text{J}}}}=c_{\text{s}}\left({\frac {\pi }{G\rho }}\right)^{\frac {1}{2}},} \)

where G is the gravitational constant, c s {\textstyle c_{\text{s}}} {\textstyle c_{\text{s}}} is the sound speed, and ρ {\textstyle \rho } {\textstyle \rho } is the enclosed mass density.

It is also the distance a sound wave would travel in the collapse time.

Jeans instability can also give rise to fragmentation in certain conditions. To derive the condition for fragmentation an adiabatic process is assumed in an ideal gas and also a polytropic equation of state is taken. The derivation is shown below through a dimensional analysis:

For adiabatic processes, \( {\displaystyle PV^{\gamma }={\text{constant}}\rightarrow V\sim P^{-{\frac {1}{\gamma }}}.} \)
For an ideal gas, \( {\displaystyle PV=nRT\Rightarrow P\cdot P^{-{\frac {1}{\gamma }}}=P^{\frac {\gamma -1}{\gamma }}\sim T\Rightarrow P\sim T^{\frac {\gamma }{\gamma -1}}.} \)
Polytropic equation of state,\( {\displaystyle P=K\rho ^{\gamma }\rightarrow T\sim \rho ^{\gamma -1}.} \)
Jeans mass, \( {\displaystyle M_{\text{J}}\sim T^{\frac {3}{2}}\rho ^{-{\frac {1}{2}}}\sim \rho ^{{\frac {3}{2}}(\gamma -1)}\rho ^{-{\frac {1}{2}}}.} \)
Thus, \( {\displaystyle M_{\text{J}}\sim \rho ^{{\frac {3}{2}}\left(\gamma -{\frac {4}{3}}\right)}.} \)

If the adiabatic index \( {\textstyle \gamma >{\frac {4}{3}}} \), the Jeans mass increases with increasing density, while if \( {\textstyle \gamma <{\frac {4}{3}}} \) the Jeans mass decreases with increasing density. During gravitational collapse density always increases,[3] thus in the second case the Jeans mass will decrease during collapse, allowing smaller overdense regions to collapse, leading to fragmentation of the giant molecular cloud. For an ideal monatomic gas, the adiabatic index is 5/3. However, in astrophysical objects this value is usually close to 1 (for example, in partially ionized gas at temperatures low compared to the ionization energy).[4] More generally, the process is not really adiabatic but involves cooling by radiation that is much faster than the contraction, so that the process can be modeled by an adiabatic index as low as 1 (which corresponds to the polytropic index of an isothermal gas)[citation needed]. So the second case is the rule rather than an exception in stars. This is the reason why stars usually form in clusters.
See also

Bonnor–Ebert mass
Langmuir waves (similar waves in a plasma)


Jeans, J. H. (1902). "The Stability of a Spherical Nebula". Philosophical Transactions of the Royal Society A. 199 (312–320): 1–53. Bibcode:1902RSPTA.199....1J. doi:10.1098/rsta.1902.0012. JSTOR 90845.
Abbasi, Amir (2018). "Effect of polarization force on the Jeans instability in collisional dusty plasmas". Plasma Science and Technology. 20 (3): 035301. Bibcode:2018PlST...20c5301A. doi:10.1088/2058-6272/aa96fa.

[Glatzmaier G.A. lecture notes, University of California, Santa Cruz, https://websites.pmc.ucsc.edu/~glatz/astr_112/lectures/notes6.pdf]

Jeans, J. H. (1902). "The Stability of a Spherical Nebula". Philosophical Transactions of the Royal Society A. 199 (312–320): 1–53. Bibcode:1902RSPTA.199....1J. doi:10.1098/rsta.1902.0012. JSTOR 90845.
Longair, Malcolm S. (1998). Galaxy Formation. Berlin: Springer. ISBN 3-540-63785-0.
Clarke, Cathie; Carswell, Bob (2007). Astrophysical Fluid Dynamics. Cambridge: Cambridge University Press. ISBN 978-0-521-85331-6.


Star formation
Object classes

Interstellar medium Molecular cloud Bok globule Dark nebula Young stellar object Protostar T Tauri star Pre-main-sequence star Herbig Ae/Be star Herbig–Haro object

Theoretical concepts

Initial mass function Jeans instability Kelvin–Helmholtz mechanism Nebular hypothesis Planetary migration

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