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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]
A star forms by accumulation of material that falls in to a protostar from a circumstellar disk or envelope. Material in the disk is cooler than the surface of the protostar, so it radiates at longer wavelengths of light producing excess infrared emission. As material in the disk is depleted, the infrared excess decreases.
W33A is a protostar located approximately 12,000 light-years away from Earth, in the constellation Sagittarius.As a star in the early stages of formation, so has attracted the interest of astronomers, who observed that while the protostar is accumulating material from surrounding clouds of gas and dust, it is simultaneously ejecting fast moving jets of particles from its north and south poles.
Pre-stellar cores are the nurseries of new stars, and are an early phase in the formation of low-mass stars, before gravitational collapse produces a central protostar.The spatial distribution of pre-stellar cores shows the history of their formation, and their sensitivity to the physics controlling their creation.
A pre-main-sequence star (also known as a PMS star and PMS object) is a star in the stage when it has not yet reached the main sequence.Earlier in its life, the object is a protostar that grows by acquiring mass from its surrounding envelope of interstellar dust and gas.
HOPS 383 is a Class 0 protostar. It is the first Class 0 protostar discovered to have had an outburst, [1] and as of 2020, the youngest protostar known to have had an outburst. [1] The outburst, discovered by the Herschel Orion Protostar Survey (HOPS) team, was first reported in February 2015 in The Astrophysical Journal Letters. [2]
In stellar evolution, an FU Orionis star (also FU Orionis object, or FUor) is a pre–main-sequence star which displays an extreme change in magnitude and spectral type. One example is the star V1057 Cyg, which became six magnitudes brighter and went from spectral type dKe to F-type supergiant during 1969-1970.