North polar sequence
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 Today it has been replaced by the UBV photometric system.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
References
External links
- Data at Google books
- Schematic images
| Formation | |
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| Evolution | |
| Luminosity class | |
| Spectral classification | |
| Remnants | |
| Hypothetical stars | |
| Nucleosynthesis | |
| Structure | |
| Properties | |
| Star systems | |
| Earth-centric observation of | |
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| Related articles | |
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