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Stars are born inside quite dense concentrations of interstellar gas and dust called molecular clouds. These regions are extremely cold and at these temperatures the gases become molecular and bind together.
Turbulance deep inside these clouds of dust causes knots with a large mass to form and the dust will begin to collapse under it’s own gravitational attraction. As the cloud collapses the material in the centre begins to heat up. This hot core is known as a protostar and will one day become a star.
As the cloud collapses, a dese hot core begins to form and it gathers dust and gas. However not all this material will become a star, the remaining dust can become planets, comets, asteroids or may just remain as dust.
In some cases the cloud may not collapse at a steady pace. In January 2004 an astronomer named James McNeil discovered a small nebula that appeared very close to the nebula Messier 78 in the constellation of Orion. When observers studied McNeil’s Nebula, they found that its brightness appears to vary. Observations with NASA’s Chandra X-ray Observatory provided an explanation- ‘the interaction between the young star's magnetic field and the surrounding gas causes episodic increases in brightness.’
Turbulance deep inside these clouds of dust causes knots with a large mass to form and the dust will begin to collapse under it’s own gravitational attraction. As the cloud collapses the material in the centre begins to heat up. This hot core is known as a protostar and will one day become a star.
As the cloud collapses, a dese hot core begins to form and it gathers dust and gas. However not all this material will become a star, the remaining dust can become planets, comets, asteroids or may just remain as dust.
In some cases the cloud may not collapse at a steady pace. In January 2004 an astronomer named James McNeil discovered a small nebula that appeared very close to the nebula Messier 78 in the constellation of Orion. When observers studied McNeil’s Nebula, they found that its brightness appears to vary. Observations with NASA’s Chandra X-ray Observatory provided an explanation- ‘the interaction between the young star's magnetic field and the surrounding gas causes episodic increases in brightness.’