Astronomy 218 Building Stars out of Gas clouds Star-Forming Regions Star formation is an ongoing process in galaxies. It is concentrated in a number of star-forming regions throughout these galaxies. Star-forming regions are associated with dark & emission nebulae. Collapsing Clouds The association with nebulae is causal, star formation occurs when part of a dust cloud contracts under its own gravitational force. Typical density in the dense core of a molecular cloud is 12 −3 nmc ~ 10 molecules m .
This equates to a mass density of ρmc = μ mp nmc. −15 −3 −12 −3 ρmc = 1.7 × 10 μ kg m = 2.9 × 10 μ M☉ AU Clearly, tremendous compression must occur to reach the −3 densities of stars. For example, ρ☉ = 1400 kg m . A molecular cloud core of a solar mass would have a radius 6 Rmc ~ 10 R☉ = 4000 AU = 0.02 pc. Collapse Time An estimate of the collapse time can be calculated from Kepler’s law. For a gas particle with orbital semimajor axis a, where M(r) is the mass interior to the particle's position. If the entire cloud is collapsing, M(r) is constant and we can consider the molecule to be on a very eccentric orbit. Then a = r0/2 and the time to reach the center, tff ~ P/2. Note that the result does not depend on the size of the cloud, r0, only the initial cloud density, ρ0. Sound Waves
This estimate of tff indicates how long collapse takes once it starts, but how does collapse start? The gas cloud is in hydrostatic equilibrium, with pressure balancing gravity. Any external push on the cloud is met by pressure waves, which travel at the speed of sound, The travel time for a wave of increased pressure to reach the surface and balance the external push is tpress ~ r0/cs.
If tpress < tff the pressure can respond to a perturbation and maintain hydrostatic equilibrium, but if tpress > tff, the equilibrium is unstable. Jean’s Length
The relationship tpress > tff leads to a limit of the size a cloud that is stable, which depends on density and temperature. A cloud larger than the Jean’s length, rJ, is prone to collapse when perturbed. For molecular hydrogen, μ = 2 & γ = 7/5. The corresponding mass is the Jean’s mass, MJ. Horsehead Nebula The Horsehead Nebula (Barnard 33), ~1 pc across and with a mass of 1000 M☉, is too large to collapse into a single star.
Instead small dense cores, with M ~ MJ within the nebula that will individually form stars. Fragmentation The first stage of star formation is the contraction of a large interstellar cloud, probably triggered by a shock or pressure wave from a nearby star. As it contracts, opacity and turbulence and gravitational instability cause the cloud fragments into smaller pieces with M ~ MJ. Star Clusters As a result of this fragmentation, stars don’t form individually, but in clusters of hundreds to thousands, like this star-forming region in the Orion Nebula Angular momentum At the large sizes of molecular gas clouds, even small rotational velocities produce significant angular momentum. For example, the Horsehead nebula as a −1 whole is rotating at ʋrot ~ 1 km s . The dense cloud core −1 rotate more slowly, ʋrot ~ 0.1 km s During the cloud’s collapse, conservation of angular momentum magnifies ʋrot