How are stars such as the Sun? What are the fundamental processes responsible for what dark diffuse interstellar cloud composed of gas and dust, it becomes much more dense luminous object? Astronomers from the United States and the European southern Observatory has made an important step on the way to understanding this fundamental question of astronomy. They undertook a detailed examination of the inner structure of small interstellar cloud known as Barnard 68 (B68).

The current structure of this cloud is supported by the same laws of physics that apply in the case of stars. The cloud is a temporary state of equilibrium when the internal gravity counteract the pressure of the gas. But this situation can't last long.

If the balance in this cloud is broken, it begins to shrink and turns into a so-called a protostar. As the compression of the density and the temperature in the cloud increased, and with them grow and compression resistance. If the mass protostar small, it can collapse at some point to stop. This forms a ball of gas of small size, which is called a brown dwarf. More massive protostar is developing differently. At a certain stage of compression density and the temperature in the center grows to such an extent that starts here thermonuclear reaction. From this moment the star can be considered to be born. Such stars, surrounded by the remains of gas and dust from which they formed, are observed in many dense gazofobija clouds in our own and other galaxies. If protostar cloud rotates at high speed, the remains of gas and dust form the young star's disk, which can be formed planetary system.

A good understanding of the processes of birth of stars and planetary systems is closely linked with detailed knowledge and understanding of the conditions inside the cold dark interstellar clouds. However, these clouds opaque, and their physical structure remained a mystery throughout that time, as it became known about their existence. Subsequent phases of the birth of such a cloud of stars known much better.

Results in studies of clouds V results changed this situation. Using new observational techniques, the researchers were able detailed probing of the internal structure of the cloud. Found that the average density increases monotonically to the center. This is consistent with the theoretical model in which isolated spherical gas cloud with some temperature of its own gravity balance internal thermal pressure. Without an accurate physical description of the structure, with very high accuracy (about 3%), you can define the basic parameters of the cloud, such as its size and the ratio of gas and dust.

New observational technique is based on measuring the radiation of the stars that are behind the clouds. Passing through the cloud, the radiation is absorbed and scattered by dust particles. This effect depends on the color (wavelength), and the stars become more red than it actually is. He also proportional to the amount of shade material, and therefore the greatest is for those stars that are located behind the Central part of the cloud. Measuring the degree of redness stars seen through different areas of the cloud, you can get a table of distribution of dust in the cloud.

But obtaining such distribution is a complex task, as even a small cloud is so opaque that through them you can see very little of the background stars. Only large telescopes and high-sensitivity devices capable of detecting a sufficient number of stars that can be achieved significant results.