Name

Eagle Nebula (M16)

Serpens

Lagoon Nebula (M8)

Sagittarius

Orion Nebula (M42)

Orion

Tarantula Nebula (NGC 2070)

Dorado

Trifid Nebula (M20)

Sagittarius

Omega Nebula (M17)

Sagittarius

radiation may also be enough to blow away lighter elements such as hydrogen. Meanwhile, the star itself continues to collapse, and may go through a period of pulsation and instability known as a "T-Tauri" phase before settling down as a main-sequence star, where it will remain for most of its life span.

strong stellar winds of charged particles

s Stellar adolescence

As the star approaches the main sequence, material from the disk continues to spiral inward. The protostar's increasingly strong magnetic field can trap some of this material and eject it at the poles.

Main sequence

The star shines steadily for most of its life. Its brightness and life span are determined by the nuclear reactions inside the star, which are governed by its composition and mass.

s Stellar adolescence

As the star approaches the main sequence, material from the disk continues to spiral inward. The protostar's increasingly strong magnetic field can trap some of this material and eject it at the poles.

Main sequence

The star shines steadily for most of its life. Its brightness and life span are determined by the nuclear reactions inside the star, which are governed by its composition and mass.

a HERBiG-HARO OBJECT

Some young stars, such as Gamma Cassiopeiae (shown here), are still embedded in nebulosity as they go through their "bipolar jet" phase, flinging off excess material. Where this material collides with the surrounding gas clouds, it causes them to glow, creating a type of emission nebula called a Herbig-Haro object.

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