The observatory was originally established at Stonyhurst College in 1838, and intended primarily to serve as a meteorological station. With the foundation of the Meteorological Office in 1854, it became one of seven key UK stations. The observatory was managed and operated by the Jesuit priests who ran the school. During the mid-nineteenth century, Fathers Weld, Perry and Sidgreaves, broadened the scope of the observatory's operations to include astronomy, geomagnetrometry and seismology.

In 1858, the observatory was chosen as one of the main observing stations by General Sir Edward Sabine, when he was conducting a magnetic survey of England. Five years later, the observatory's first regular series of monthly geomagnetic observations was inaugurated by Fr Sidgreaves. In 1866, the latter installed a set of self-recording photographic magnetographs, donated by the Royal Society, in a specially constructed underground chamber.

Sidgreaves also carried out original research into the solar spectrum, contained in many papers published in the Monthly Notices of the Royal Astronomical Society. In solar physics he made a long photographic study of the Sun, including hundreds of photographs taken in the violet light of calcium, using a Hilger spectroscope acquired by Father Perry. In this research he showed that the Sun is spectroscopically, a variable star.

During his time as president of the Branch, Sidgreaves carried out original work into the spectroscopy of novae. His work on Nova Aurigae, in 1892, contained some of the first photographs of the spectra of novae ever taken. He recognised in them the similarity between the spectrum of the new star and that of the solar chromosphere, rich in the pink light of ionised hydrogen. Equally significant results were obtained with the spectrum of Nova Perseii, in 1901.

Sidgreaves was particularly interested in the connection between sunspots and fluctuations in Earth's magnetic field. He published several papers on the subject based on observations made at Stonyhurst. In work carried out between 1881 and 1898, he came to the conclusion that although magnetic storms were not directly a result of sunspots, they were due to clouds of electrified particles moving between the Sun and Earth. It is now known that solar mass ejections caused by solar flares can interact with the Earth's magnetic field to produce magnetic storms. They are now of great importance, having been known to disrupt national power-grids and cause expensive damage to Earth-orbiting telecommunication satellites.

In 1848, the year in which Sidgreaves first attended the College, the Italian astronomer, Father Angelo Secchi, of the Jesuit Collegio di Romano Observatory, in Rome, had stayed at Stonyhurst, in retreat from revolutionary troubles in Italy. Stonyhurst's astronomical leanings, particularly in solar observation, apparently stemmed from his time in residence.

The 'Stonyhurst System of heliographic coordinates' is one of two 'heliographic coordinate' systems used for identifying the position of features on the Sun's surface. In the Stonyhurst system the zero point is set at the intersection of the Sun's equator and central meridian as seen from the Earth. Longitude increases towards the Sun's western limb. A solar feature will have a fixed latitude as it rotates across the solar disk, but its longitude will increase. This is in contrast to the Carrington heliographic coordinate system, where the longitude remains approximately fixed in time. The coordinates take their name from the College where they were devised in the nineteenth century.^[8]

A 'Stonyhurst disk' is used to determine the longitude and latitude of sunspots. The Earth doesn't orbit precisely around the Sun's equator, so through the year the center of solar pictures moves up and down a little more than 7 degrees. This angle varies sinusoidally through the year and is called B0. Earth crosses the Sun's equator about December 7 and June 7 each year. This means that the lines of latitude on the sun do not appear as lines from the Earth, but as elliptical arcs. Sunspots and other features will rotate across the face of the Sun along lines of latitude. Stonyhurst disks are transparent overlays that match the size of whole-disk images of the Sun. These disks provide a graphic means of locating sunspots on the solar disk in reference to lines of latitude and longitude. Different disk overlays are produced for different dates.^[9]

• Muir, T.E. (2006) Stonyhurst, (St Omers Press, Gloucestershire) second edition ISBN 0-9553592-0-1

• Stonyhurst College website
• Article on the observatory
• Virtual tour
• Meteogroup entry
• Met Office entry
• Stonyhurst Refractor
• 1927 eclipse at Stonyhurst 1
• 1927 eclipse at Stonyhurst 2
• Article on 1927 eclipse at Stonyhurst
• BBC Two programme featuring the Stonyhurst Observatory