Carrington rotations
Convert a date to its Carrington rotation number and back, and browse rotation start and end times.
CR 655
| Start | September 12, 1902 at 08:56 PM UTC |
|---|---|
| End | October 10, 1902 at 03:36 AM UTC |
| Length (days) | 27.28 |
Neighbouring rotations
| CR | Start | End | Length (days) |
|---|---|---|---|
| 650 | April 29, 1902 at 06:34 PM UTC | May 26, 1902 at 11:54 PM UTC | 27.22 |
| 651 | May 26, 1902 at 11:54 PM UTC | June 23, 1902 at 04:40 AM UTC | 27.20 |
| 652 | June 23, 1902 at 04:40 AM UTC | July 20, 1902 at 09:30 AM UTC | 27.20 |
| 653 | July 20, 1902 at 09:30 AM UTC | August 16, 1902 at 02:52 PM UTC | 27.22 |
| 654 | August 16, 1902 at 02:52 PM UTC | September 12, 1902 at 08:56 PM UTC | 27.25 |
| 655 | September 12, 1902 at 08:56 PM UTC | October 10, 1902 at 03:36 AM UTC | 27.28 |
| 656 | October 10, 1902 at 03:36 AM UTC | November 6, 1902 at 10:42 AM UTC | 27.30 |
| 657 | November 6, 1902 at 10:42 AM UTC | December 3, 1902 at 06:11 PM UTC | 27.31 |
| 658 | December 3, 1902 at 06:11 PM UTC | December 31, 1902 at 02:02 AM UTC | 27.33 |
| 659 | December 31, 1902 at 02:02 AM UTC | January 27, 1903 at 10:10 AM UTC | 27.34 |
| 660 | January 27, 1903 at 10:10 AM UTC | February 23, 1903 at 06:19 PM UTC | 27.34 |
About this tool
A Carrington rotation is the time the Sun takes to turn once on its axis as seen from the Earth: 27.2753 days on average. The count was defined by the English astronomer Richard Carrington, who studied sunspots in the 1850s; rotation 1 began on 9 November 1853, and the numbering has run without interruption since.
Explorer computes the start of each rotation with the formula given by Jean Meeus in Astronomical Algorithms (chapter 29), implemented in its own astronomy library and checked against published dates. A rotation begins when the Carrington longitude L₀ of the central meridian passes through 0°; because the Earth moves along its orbit, the synodic period varies slightly around the mean, hence lengths of 27.2 to 27.3 days.
Observers use the rotation number as a calendar for the Sun: an active region that crosses the disc reappears about one rotation later, and the community activity heatmap shows one row per rotation so that returning regions line up. Enter a date to find its rotation, or a number to get the UTC start and end dates and the neighbouring rotations.