Everything about Star Formation totally explained
Star Formation is the process by which dense parts of
molecular clouds collapse into a ball of
plasma to form a
star. As a branch of
astronomy star formation includes the study of the
interstellar medium and
giant molecular clouds as precursors to the star formation process and the study of
young stellar objects and
planet formation as its immediate products. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of
binary stars and the
initial mass function.
Theoretical Outline
According to current theories of star formation, cores of molecular clouds (regions of especially high density) become gravitationally unstable, fragment, and begin to
collapse (the so-called
spontaneous star formation), or shockwaves from
supernovae or other energetic astronomical processes trigger star formation in nearby nebulae (the so-called
triggered star formation). Part of the gravitational energy lost in this collapse is radiated in the
infrared, with the remainder increasing the temperature of the core of the object. The accretion of material happens partially through a
circumstellar disc. When the density and temperature are high enough,
deuterium fusion ignition occurs, and the outward
pressure of the resultant radiation slows (but doesn't stop) the collapse. Material comprising the cloud continues to "rain" onto the
protostar. In this stage bipolar flows are produced, probably an effect of the
angular momentum of the infalling material. Finally,
hydrogen begins to fuse in the core of the star, and the rest of the enveloping material is cleared away.
The protostar follows a
Hayashi track on the
Hertzsprung-Russell diagram. The contraction will proceed until the
Hayashi limit is reached, and thereafter contraction will continue on a
Kelvin-Helmholtz timescale with the temperature remaining stable. Stars with less than 0.5
solar masses thereafter join the main sequence. For more massive protostars, at the end of the Hayashi track that'll slowly collapse in near hydrostatic equilibrium, following the
Henyey track.
The stages of the process are well defined in stars with masses around one
solar mass or less. In high mass stars, the length of the star formation process is comparable to the other timescales of their evolution, much shorter, and the process isn't so well defined. The later evolution of stars are studied in
stellar evolution.
Observations
Key elements of star formation are only available by observing in
wavelengths other than the
optical. The structure of the molecular cloud and the effects of the protostar can be observed in near-IR extinction maps (where the number of stars are counted per unit area and compared to a nearby zero extinction area of sky), continuum dust emission and
rotational transitions of
CO and other molecules; these last two are observed in the millimeter and
submillimeter range. The radiation from the protostar and early star has to be observed in
infrared astronomy wavelengths, as the
extinction caused by the rest of the cloud in which the star is forming is usually too big to allow us to observe it in the visual part of the spectrum. This presents considerable difficulties as the atmosphere is almost entirely opaque from 20μm to 850μm, with narrow windows at 200μm and 450μm. Even outside this range atmospheric subtraction techniques must be used.
The formation of individual stars can only be directly observed in
our Galaxy, but in distant galaxies star formation has been detected through its unique
spectral signature.
Notable Pathfinder Objects
- MWC 349 was first discovered in 1978, and is estimated to be only 1,000 years old. Since the object is located at a distance of 10,000 lightyears, it actually is now 11,000 years old.
- VLA 1623 -- The first exemplar Class 0 protostar, a type of embedded protostar that has yet to accrete the majority of its mass. Found in 1993, is possibly younger than 10,000 years (External Link
).
- L1014 -- An incredibly faint embedded object representative of a new class of sources that are only now being detected with the newest telescopes. Their status is still undetermined, they could be the youngest low-mass Class 0 protostars yet seen or even very low-mass evolved objects (like a brown dwarf or even an interstellar planet). (External Link).
- IRS 8* -- The youngest known main sequence star, discovered in August 2006. It is estimated to be 3.5 million years old (External Link).
Low Mass and High Mass Star Formation
Stars of different masses are thought to form by slightly different mechanisms. The theory of low-mass star formation, which is well-supported by a plethora of observations, suggests that low-mass stars form by the gravitational collapse of rotating density enhancements within molecular clouds. As described above, the collapse of a rotating cloud of gas and dust leads to the formation of an accretion disk through which matter is channeled onto a central protostar. For stars with masses higher than about 8 solar masses, however, the mechanism of star formation isn't well understood.
Massive stars emit copious quantities of radiation which pushes against infalling material. In the past, it was thought that this
radiation pressure might be substantial enough to halt accretion onto the massive protostar and prevent the formation of stars with masses more than a few tens of solar masses. Recent theoretical work has shown that the production of a jet and outflow clears a cavity through which much of the radiation from a massive protostar can escape without hindering accretion through the disk and onto the protostar. Present thinking is that massive stars may therefore be able to form by a mechanism similar to that by which low mass stars form.
There is mounting evidence that at least some massive protostars are indeed surrounded by accretion disks. Several other theories of massive star formation remain to be tested observationally. Of these, perhaps the most prominent is the theory of competitive accretion, which suggests that massive protostars are "seeded" by low-mass protostars which compete with other protostars to draw in matter from the entire parent molecular cloud, instead of simply from a small local region.
Another theory of massive star formation suggests that massive stars may form by the coalescence of two or more stars of lower mass.
Further Information
Get more info on 'Star Formation'.
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