Bonnor–Ebert mass

In astrophysics, the Bonnor–Ebert mass is the largest mass that an isothermal gas sphere embedded in a pressurized medium can have while still remaining in hydrostatic equilibrium. Clouds of gas with masses greater than the Bonnor–Ebert mass must inevitably undergo gravitational collapse to form much smaller and denser objects.[1][2] As the gravitational collapse of an interstellar gas cloud is the first stage in the formation of a protostar, the Bonnor–Ebert mass is an important quantity in the study of star formation.[3]

For a gas cloud embedded in a medium with a gas pressure ${\displaystyle p_{0}}$, the Bonnor–Ebert mass is given by[4]

${\displaystyle M_{BE}(p_{0})={225 \over {32{\sqrt {5\pi }}}}{c_{s}^{4} \over {(aG)}^{3/2}}{1 \over {\sqrt {p_{0}}}}}$

where G is the gravitational constant and ${\displaystyle c_{s}\equiv {\sqrt {kT/{\mu m_{H}}}}}$ is the isothermal sound speed (${\displaystyle \gamma =1}$) with ${\displaystyle \mu }$ as the molecular mass. ${\displaystyle a}$ is a dimensionless constant which varies based on the density distribution of the cloud. For a uniform mass density ${\displaystyle a=1}$ and for a centrally peaked density ${\displaystyle a\approx 1.67}$.[5]

See also

• Jeans mass

References

1. Ebert, Rolf (1955). "Über die Verdichtung von H I-Gebieten". Zeitschrift für Astrophysik. 37: 217. Bibcode:1955ZA.....37..217E.
2. Bonnor, William Bowen (1956). "Boyle's Law and gravitational instability". Monthly Notices of the Royal Astronomical Society. 116: 351. Bibcode:1956MNRAS.116..351B. doi:10.1093/mnras/116.3.351.
3. Carroll, Bradley W.; Ostlie, Dale A. (2007). An Introduction to Modern Astrophysics. Addison-Wesley. pp. 413–414.
4. Draine, Bruce (2011). Physics of the Interstellar and Intergalactic Medium. Oxfordshire United Kingdom: Princeton University Press. p. 457. ISBN 978-0-691-12214-4.
5. Draine, Bruce (2011). Physics of the Interstellar and Intergalactic Medium. Oxfordshire United Kingdom: Princeton University Press. p. 456. ISBN 978-0-691-12214-4.