Cloud collapse
Stellar cluster and star-forming region M 17.

An interstellar cloud of gas will remain in hydrostatic equilibrium as long as the kinetic energy of the gas pressure is in balance with the potential energy of the internal gravitational force. Mathematically this is expressed using the virial theorem, which states that, to maintain equilibrium, the gravitational potential energy must equal twice the internal thermal energy.[14] If a cloud is massive enough that the gas pressure is insufficient to support it, the cloud will undergo gravitational collapse. The mass above which a cloud will undergo such collapse is called the Jeans mass. The Jeans mass depends on the temperature and density of the cloud, but is typically thousands to tens of thousands of solar masses.[2] This coincides with the typical mass of an open cluster of stars, which is the end product of a collapsing cloud.[15]

In triggered star formation, one of several events might occur to compress a molecular cloud and initiate its gravitational collapse. Molecular clouds may collide with each other, or a nearby supernova explosion can be a trigger, sending shocked matter into the cloud at very high speeds.[2] Alternatively, galactic collisions can trigger massive starbursts of star formation as the gas clouds in each galaxy are compressed and agitated by tidal forces.[16] The latter mechanism may be responsible for the formation of globular clusters.[17]

A supermassive black hole at the core of a galaxy may serve to regulate the rate of star formation in a galactic nucleus. A black hole that is accreting infalling matter can become active, emitting a strong wind through a collimated relativistic jet. This can limit further star formation. However, the radio emissions around the jets may also trigger star formation. Likewise, a weaker jet may trigger star formation when it collides with a cloud.[18]

As it collapses, a molecular cloud breaks into smaller and smaller pieces in a hierarchical manner, until the fragments reach stellar mass. In each of these fragments, the collapsing gas radiates away the energy gained by the release of gravitational potential energy. As the density increases, the fragments become opaque and are thus less efficient at radiating away their energy. This raises the temperature of the cloud and inhibits further fragmentation. The fragments now condense into rotating spheres of gas that serve as stellar embryos.[19]

Complicating this picture of a collapsing cloud are the effects of turbulence, macroscopic flows, rotation, magnetic fields and the cloud geometry. Both rotation and magnetic fields can hinder the collapse of a cloud.[20][21] Turbulence is instrumental in causing fragmentation of the cloud, and on the smallest scales it promotes collapse.[22]

Bintang akan menjadi Brown Dwarf

Brown Dwarf adalah tipe bintang yang gagal melakukan reaksi nuklir untuk mengubah Hidrogen menjadi Helium seperti Matahari kita. Hal ini disebabkan karena massanya yang kurang.
Perbandingan Brown Dwarf

Akan Menjadi Red Dwarf

Akan melepaskan lapisan terluar dari bintang dengan Pulsating and Stelar Winddan meninggalkan lapisan terdalam dari inti matahari

Akan terjadi Supernova
Tipe-Tipe Supernova

a. Type II Supernova
Supernova ini terjadi pada bintang yang memiliki 8-50 kali massa matahari. Ledakan ini terjadi secara cepat dan menghasilkan ledakan yang sangat kuat



b. Type Ia Supernova
Supernova ini terjadi pada tata surya dengan bintang ganda, dimana bintang yang lebih kecil menabrak/terserap ke bintang induk. Sehingga terjadi kenaikan suhu matahari yang mendadak dan akhirnya bintang tidak mampu menahan temperatur yang terjadi.


c. Type 1b Supernova
Terjadi akibat hancurnya inti bintang pada matahari yang sangat masive