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Large disks are routinely observed in many star-forming regions such as the Orion nebula. [18] Artist's impression of the disc and gas streams around young star HD 142527. [53] The lifespan of the accretion disks is about 10 million years. [17] By the time the star reaches the classical T-Tauri stage, the disk becomes thinner and cools. [45]
A protostar is a very young star that is still gathering mass from its parent molecular cloud.It is the earliest phase in the process of stellar evolution. [1] For a low-mass star (i.e. that of the Sun or lower), it lasts about 500,000 years. [2]
NGC 7538, near the more famous Bubble Nebula, is located in the constellation Cepheus. It is located about 9,100 light-years from Earth. It is home to the biggest yet discovered protostar which is about 300 times the size of the Solar System. [4] It is located in the Perseus Arm of the Milky Way and is probably part of the Cassiopeia OB2 ...
In astronomy or planetary science, the frost line, also known as the snow line or ice line, is the minimum distance from the central protostar of a solar nebula where the temperature is low enough for volatile compounds such as water, ammonia, methane, carbon dioxide and carbon monoxide to condense into solid grains, which will allow their accretion into planetesimals.
These objects represent the final stage before a planetary nebula. During this stage, the red giant star begins to slowly expel its outermost layers of material. A protoplanetary nebula usually glows by reflecting the light from its parent star. This stage is usually brief, typically lasting no more than a few thousand years.
NGC 6357 is a diffuse nebula near NGC 6334 in the constellation Scorpius. The nebula contains many proto-stars shielded by dark discs of gas, and young stars wrapped in expanding "cocoons" or expanding gases surrounding these small stars. It is also known as the Lobster Nebula.
It is associated with a dark cloud L1450 (Barnard 205). Estimates of the distance to this nebula range from 980–1,140 ly (300–350 pc). [4] This nebula is in the western part [4] of the Perseus molecular cloud and is a young region of very active star formation, [6] being one of the best-studied objects of its type. [4]
Over about 100,000 years, [9] the competing forces of gravity, gas pressure, magnetic fields, and rotation caused the contracting nebula to flatten into a spinning protoplanetary disc with a diameter of about 200 AU [11] and form a hot, dense protostar (a star in which hydrogen fusion has not yet begun) at the centre. [25]