# data[].attributes.body
At this stage, gaseous Hydrogen and Helium begins to condense as gravity pulls the elements together. An example of this structure is the Eagle Nebula which is shown in the photo of this step.

# data[].attributes.body
At this stage, the nebula collapses due to gravity to form an accretion disk and a condensed mass in the center. A star in its very early stages emerges. These structures contain disks and long jets that emerge from the proto-star. An example of this is Herbig-Haro 34 (HH-34), a proto-star very early in its development.

# data[].attributes.body
The proto-star officially emerges as a star when hydrostatic equilibrium occurs. This is the balance of forces of gravity and fusion, creating a stability in the star. An example of a star is Betelgeuse.

# data[].attributes.body
Main Sequence is the stage of most of a star’s life. It describes when the star is at hydrostatic equilibrium and is burning hydrogen into helium through fusion. An example of a star in main sequence is our very own Sun, which is about 4.6 billion years old.

# data[].attributes.body
As more hydrogen is burned into helium, the core of the sun contracts greatly. This makes the sun larger and more red as a result. An example of a red giant is Aldebaran

# data[].attributes.body
This is the death of the star, and the formation of a white dwarf and a planetary nebula. What happens is the core collapses and the outer materials simply expel outward. An example of this is the binary star of NGC 6326 which had once gone through a low mass death.

# data[].attributes.headline
Step 7: White Dwarf and Planetary Nebula

# data[].attributes.subject
Step 7: White Dwarf and Planetary Nebula

# data[].attributes.body
The matter of the death expels outward forming a nebula like structure. The remains of the core is now a white dwarf star which is very dim and dense. An example of a white dwarf is Sirius B.