| Display title | Astronomy:Wilson–Bappu effect |
| Default sort key | Wilson-Bappu Effect |
| Page length (in bytes) | 5,867 |
| Namespace ID | 3024 |
| Namespace | Astronomy |
| Page ID | 605261 |
| Page content language | en - English |
| Page content model | wikitext |
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| Page creator | imported>CodeMe |
| Date of page creation | 08:37, 6 February 2024 |
| Latest editor | imported>CodeMe |
| Date of latest edit | 08:37, 6 February 2024 |
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Description | Content |
Article description: (description)
This attribute controls the content of the description and og:description elements. | The Ca II K line in cool stars is among the strongest emission lines which originates in the star's chromosphere. In 1957, Olin C. Wilson and M. K. Vainu Bappu reported on the remarkable correlation between the measured width of the aforementioned emission line and the absolute visual magnitude of the... |
