Carrington rotations
Convert a date to its Carrington rotation number and back, and browse rotation start and end times.
CR 763
| Start | October 6, 1910 at 02:21 PM UTC |
|---|---|
| End | November 2, 1910 at 09:25 PM UTC |
| Length (days) | 27.29 |
Neighbouring rotations
| CR | Start | End | Length (days) |
|---|---|---|---|
| 758 | May 23, 1910 at 10:54 AM UTC | June 19, 1910 at 03:43 PM UTC | 27.20 |
| 759 | June 19, 1910 at 03:43 PM UTC | July 16, 1910 at 08:30 PM UTC | 27.20 |
| 760 | July 16, 1910 at 08:30 PM UTC | August 13, 1910 at 01:47 AM UTC | 27.22 |
| 761 | August 13, 1910 at 01:47 AM UTC | September 9, 1910 at 07:45 AM UTC | 27.25 |
| 762 | September 9, 1910 at 07:45 AM UTC | October 6, 1910 at 02:21 PM UTC | 27.27 |
| 763 | October 6, 1910 at 02:21 PM UTC | November 2, 1910 at 09:25 PM UTC | 27.29 |
| 764 | November 2, 1910 at 09:25 PM UTC | November 30, 1910 at 04:51 AM UTC | 27.31 |
| 765 | November 30, 1910 at 04:51 AM UTC | December 27, 1910 at 12:38 PM UTC | 27.32 |
| 766 | December 27, 1910 at 12:38 PM UTC | January 23, 1911 at 08:45 PM UTC | 27.34 |
| 767 | January 23, 1911 at 08:45 PM UTC | February 20, 1911 at 04:55 AM UTC | 27.34 |
| 768 | February 20, 1911 at 04:55 AM UTC | March 19, 1911 at 12:40 PM UTC | 27.32 |
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.