This critical mass is known as the Jeans mass. It ends when the infalling gas is depleted, leaving a pre-main-sequence star, which contracts to later become a main-sequence star at the onset of hydrogen fusion producing helium. The actual radiation emanating from a protostar is predicted to be in the infrared and millimeter regimes.
As the dense core accrues mass from its larger, surrounding cloud, self-gravity begins to overwhelm pressure, and collapse begins. Jump to: navigation, search. Protostar. The shrinkage of the protostar increases the self gravity.
Protostar. As the cloud continues to contract it begins to increase in temperature. See more. Exactly how material in the disk spirals inward onto the protostar is not yet understood, despite a great deal of theoretical effort. A protostar becomes a main sequence star when its core temperature exceeds 10 million K. This is the temperature needed for hydrogen fusion to operate efficiently.  The phase begins when a molecular cloud fragment first collapses under the force of self-gravity and an opaque, pressure supported core forms inside the collapsing fragment. This is not caused by nuclear reactions but by the conversion of gravitational energy to thermal kinetic energy. This problem is illustrative of the larger issue of accretion disk theory, which plays a role in much of astrophysics. An object can be considered a protostar as long as material is still falling inward. It can take a protostar millions of years to complete this early stage of stellar evolution. A new star, or protostar, does not yet shine. When the temperature of a protostar reaches 10 million°K, or about 18 million°F (10 million°C), it stops contracting. A person can't be created overnight, completely ready for the adult world. Protostar. A protostar has a simple evolution, because it has a simple internal structure. These turbulent velocities compress the gas in shocks, and generates filaments and clumpy structures within the giant molecular cloud over a wide range of sizes and densities. The more the cloud contracts the more the temperature increases. The protostar period is the period in the evolution of a star after the cloud of hydrogen, helium and dust has started contraction and before the star has reached the main sequence on the Hertzsprung-Russell diagram. The phase begins when a molecular cloud fragment first collapses under the force of self-gravity and an opaque, pressure supported core forms inside the collapsing fragment.
This can be explained if it is assumed that as a cloud contracts it does not do so uniformly.
is a baby star, an area of material that hasn't yet formed into a fully-fledged star. For a low mass star (i.e.
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