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Beta Ceti:
Giant Star's Corona Brightens with Age

Beta Ceti
Credit: NASA/CXC

Beta Ceti is a bright, giant star with a hot corona that radiates about 2,000 times more X-ray power than the Sun. Scientists suspect that this X-ray activity is somehow related to its advanced stage of evolution called core helium burning. During this stage, the core of the star is very hot (more than a hundred million degrees Celsius) and converting helium to carbon via nuclear fusion reactions.

Using the theory of how stars evolve, we can reconstruct the history of Beta Ceti, a star with a mass of about 3 Suns. Over the first billion years of its existence, Beta Ceti was powered by nuclear fusion reactions converting hydrogen to helium in the core.

After the hydrogen in the core was exhausted, the central region of the star contracted until hydrogen gas around the helium core became hot and dense enough for hydrogen fusion reactions to ignite there. This powerful new energy source caused the outer regions of the star to expand greatly and cool. At this point Beta Ceti became a red giant. During the red giant phase, Beta Ceti would have been a very weak X-ray source.

After about 10 million years, the core of the star contracted and heated to more than 100 million degrees, enabling helium fusion reactions to occur there. In this core helium burning stage, which will last 100 million years or more, the overall diameter of the star has shrunk to about 20 times that of the Sun and the surface temperature has increased, so it is no longer a red giant star.

Fast Facts for Beta Ceti:
Credit  NASA/CXC
Scale  Image is 1 arcmin across.
Category  Normal Stars & Star Clusters
Coordinates (J2000)  RA 00h 43m 35.40s | Dec -17° 59' 11.80"
Constellation  Cetus
Observation Dates  June 29, 2001
Observation Time  24 hours
Obs. IDs  974
Color Code  Intensity
Instrument  ACIS
Distance Estimate  95 light years
Release Date  December 30, 2004