Fall of Stellar Bodies

A report by:

RAdm. R.M. Wey and FCapt. D.L. Wey

of the office of scientific research

Much research has been conducted by this office in the area of stellar evolution, yet many questions have yet to be answered. For instance, what are the early stages of stellar formation? What determines whether a cloud of gaseous material will contain the elements to form stars, etceteras?

The early stages of stellar formation occur when interstellar clouds of gas and dust[referred to as nebula]begin to collapse. This is usually accomplished in two stages of rapid contraction[referred to as dynamic collapse]. During these periods, it is possible that fragmentation into several protostars may occur. However, this depends on such variables as its size and rate of rotation.

An interstellar cloud can be as large as one hundred times the mass of earth’s sun, and can possess angular momentum more than 10⁵ times that of its eventual progeny. The cluster NGC 2264 is known to contain adolescent stars as well as bodies still in the earliest stages of formation.

A stationary stellar dust cloud is bombarded by the radiation from other neighboring stellar bodies, this[in turn]heats up the material within the cloud. This rise in temperature also effects the gravitational forces within the cloud, causing the cloud to compress and collapse.

As the density of the cloud increases, its temperature begins to drop as ultraviolet radiation is blocked. At this point, the cloud enters an ‘isothermal phase’ in which the temperature attains a level of ten degrees Kelvin; As it continues to collapse, it moves thorough various densities[from approximately 10⁵ to 10¹¹ atoms per cubic centimeter].

As the cloud grows smaller and attains more density, its gravitational forces increase in strength, eventually overcoming the thermal pressures within. The end result is the continuing collapse of matter in the center of the cloud. When the central regions of the cloud formation become dense enough to block infrared radiation, the dynamic collapse ceases[this happens at about 100 degrees Kelvin at a density of 10¹⁴ atoms PCC(per cubic centimeter)].

At this point the region at where the collapse has ceased has a radius of approximately five astronomical units[or 465 million miles]and is referred to as ‘the first core.’ As this process continues, the temperature of the cloud reaches about two thousand degrees Kelvin with a density of approximately 10¹⁶ atoms PCC, and the diatomic hydrogen begin to break down into elemental hydrogen.

There is a period of quasi equilibrium that occurs after the first and second dynamic collapses; During these periods of semi stability, protostars go through various phases on the path to main sequence.

During this process, the temperature in the first core begins to drop; As a result, it enters a second dynamic collapse in which it reaches a density of approximately 10²⁴ atoms PCC and temperatures rise to around one hundred thousand degrees Kelvin. Due to the rise in pressure, a second core is formed, it is into this that the remaining cloud materials continue to fall. The first core having evolved into a protostar, now enters into its main sequence of stellar evolution.

Another means of stellar formation is found in the rapid rotation of dense cloud material in a series of stages. The first: matter is driven by gravitational forces along its axis of rotation. As this momentum builds, the centrifugal forces at work cause the materials in the center to begin collapse inward more rapidly. Materials in the outer regions collapse slower as the gravitational forces are spent keeping them in orbit around the center.

As a result, the material along the axis collapses faster, thereby causing the once spherical cloud to begin to flatten. Inevitably, this flattening of the disk produces the formation of a ring. Yet, at the same time, material from outside the center continues to fall, gathering speed as it does. This continues until the protosystem attains a density factor of 10²⁴ and a temperature factor of 10⁶ [in order for ignition of the protostar to main sequence], or the protosystem splits into smaller protostar groups.

It has been theorized that the Sol system was the end result of the death of a binary protostar system. This is considered possible if the angular momentum was transferred OUTWARD during part of the systems formation, or that the protostars had already reached equilibrium, and merely merged to form what would become the Sol systems present sun.

At the same time that the protostar forms, the outer regions are beginning to flatten out and cohese into what will evolve into planetary bodies. Perhaps, as did the Sol system, one or more will evolve to support life. However, such observations will require more research to confirm.