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North polar sequence

From Wikipedia, the free encyclopedia

The North polar sequence is a group of 96 stars that was used to define stellar magnitudes and colors.[1] The cluster of stars lies within two degrees of the Northern Celestial pole.[1] That fact makes them visible to everyone in the northern hemisphere.[2]

Originally proposed by Edward Charles Pickering, the system was used between 1900 and 1950. Today it has been replaced by the UBV photometric system.

See also

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References

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  1. ^ a b "North Polar Sequence - Oxford Reference".
  2. ^ "eSky: North Polar Sequence". www.glyphweb.com.

Further reading

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