Sigma Orionis

. The brighter stars are Alnitak and Alnilam. σ Orionis is a naked eye star at the eastern end of Orion's Belt, and has been known since antiquity, but it was not included in Ptolemy's Almagest. It was referred to by Al Sufi, but not formally listed in his catalogue. In more modern times, it was measured by Tycho Brahe and included in his catalogue. In Kepler's extension it is described as "Quae ultimam baltei praecedit ad austr." (preceding the outermost of the belt, to the south). It was then recorded by Johann Bayer in his Uranometria as a single star with the Greek letter σ (sigma). He described it as "in enſe, prima" (in the sword, first). It was also given the Flamsteed designation 48. In 1776, Christian Mayer described σ Ori as a triple star, having seen components AB and E, and suspected another between the two. Component D was confirmed by FGW Struve who also added a fourth (C), published in 1876. In 1892 Sherburne Wesley Burnham reported that σ Ori A was itself a very close double, although a number of later observers failed to confirm it. In the second half of the twentieth century, the orbit of σ Ori A/B was solved and at the time was one of the most massive binaries known. σ Ori A was discovered to have a variable radial velocity in 1904, considered to indicate a single-lined spectroscopic binary. The spectral lines of the secondary were elusive and often not seen at all, possibly because they are broadened by rapid rotation. There was confusion over whether the reported spectroscopic binary status actually referred to the known visual companion B. Finally in 2011, it was confirmed that the system is triple, with an inner spectroscopic pair and a wider visual companion. σ Ori E was identified as helium-rich in 1956, having variable emission features in 1974, having an abnormally strong magnetic field in 1978, and formally classified as a variable star in 1979. In 1996, a large number of low-mass pre-main sequence stars were identified in the region of Orion's Belt. A particular close grouping was discovered to lie around σ Orionis. A large number of brown dwarfs were found in the same area and at the same distance as the bright σ Orionis stars. Optical, infrared, and x-ray objects in the cluster, including 115 non-members lying in the same direction, were listed in the Mayrit Catalogue with a running number, except for the central star which was listed simply as Mayrit AB. ==Cluster==

The σ Orionis cluster is part of the Ori OB1b stellar association, commonly referred to as Orion's Belt. The cluster was not recognised until 1996 when a population of pre-main sequence stars was discovered around σ Ori. Since then it has been extensively studied because of its closeness and the lack of interstellar extinction. It has been calculated that star formation in the cluster began 3 million years (myr) ago and it is approximately 360 pc away. In the central arc-minute of the cluster five particularly bright stars are visible, labelled A to E in order of distance from the brightest component σ Ori A. The closest pair AB are only separated by 0.2" - 0.3" but were discovered with a 12" telescope. An infrared and radio source, IRS1, 3.3" from σ Ori A that was considered to be a patch of nebulosity has been resolved into two subsolar stars. There is an associated variable x-ray source that is assumed to be a T Tauri star. • HD 37699, an outlying B5 giant very close to the Horsehead Nebula • HD 37525, a B5 main sequence star and spectroscopic binary • HD 294271, a B5 young stellar object with two low mass companions • HD 294272, a binary containing two B class young stellar objects • HD 37333, a peculiar A1 main sequence star • HD 37564, an A8 young stellar object • V1147 Ori, a B9.5 giant and α2 CVn variable • HD 37686, a B9.5 main sequence star close to HD 37699 • HD 37545, an outlying B9 main sequence • HD 294273, an A8 young stellar object • 2MASS J05374178-0229081, an A9 young stellar object HD 294271 and HD 294272 make up the "double" star Struve 761 (or STF 761). It is three arc minutes from σ Orionis, which is also known as Struve 762. Over 30 other probable cluster members have been detected within an arc minute of the central star, mostly brown dwarfs and planetary mass objects such as S Ori 60, but including the early M red dwarfs 2MASS J05384746-0235252 and 2MASS J05384301-0236145. In the past a few T-dwarfs were thought to be part of the cluster, but so far most of these T-dwarfs turned out to be brown dwarfs in the foreground. Some of these L-dwarfs (around 29%) are surrounded by a dusty disk. The cluster also contains a pair consisting out of the brown dwarf SE 70 and the planetary-mass object S Ori 68, which are separated by 1700 astronomical units. In 2024 high-resolution imaging with ALMA of K-stars and early M-stars showed gaps and rings in the disks around these stars. One star called Haro 5-34 (SO 1274, K7-type star) showed five gaps, seemingly arranged in a resonant chain. The disks in the cluster are small, either due to external photoevaporation by σ Orionis or the intermediate age of the region. ==σ Orionis AB==

The brightest member of the σ Orionis system appears as a late O class star, but is actually made up of three stars, designated Aa, Ab, and B. The inner pair complete a highly eccentric orbit every 143 days, while the outer star completes its near-circular orbit once every 157 years. It has not yet completed a full orbit since it was first discovered to be a double star. All three are very young main sequence stars with masses between . Components The primary component Aa is the class O9.5 star, with a temperature of 35,000 K and a luminosity over . Lines representing a B0.5 main sequence star have been shown to belong to its close companion Ab, which has a temperature of 31,000 K and a luminosity of . Their separation varies from less than half an astronomical unit to around two AU. Although they cannot be directly imaged with conventional single mirror telescopes, their respective visual magnitudes have been calculated at 4.61 and 5.20. Ages Comparison of the observed or calculated physical properties of each star with theoretical stellar evolutionary tracks allows the age of the star to be estimated. The estimated ages of the components Aa, Ab, and B, are respectively Myr, Myr, and Myr. Within their large margins of error, these can all be considered to be consistent with each other, although it is harder to reconcile them with the 2-3 Myr estimated age of the σ Orionis cluster as a whole. ==σ Orionis C==

The faintest member of the main σ Orionis stars is component C. It is also the closest to σ Ori AB at 11", corresponding to 3,960 astronomical units. It is an A-type main sequence star. σ Ori C has a faint companion 2" away, referred to as Cb and MAD-4. Cb is five magnitudes fainter than σ Ori Ca at infrared wavelengths, K band magnitude 14.07, and is likely to be a brown dwarf. ==σ Orionis D==

Component D is a fairly typical B2 main sequence star of magnitude 6.62. It is 13" from σ Ori AB, corresponding to 4,680 AU. Its size, temperature, and brightness are very similar to σ Ori E but it shows none of the unusual spectral features or variability of that star. ==σ Orionis E==

for V1030 Orionis, plotted from TESS data Component E is an unusual variable star, classified as an SX Arietis variable and also known as V1030 Orionis. It is helium-rich, has a strong magnetic field, and varies between magnitudes 6.61 and 6.77 during a 1.19 day period of rotation. It has a spectral type of B2 Vpe. The variability is believed to be due to large-scale variations in surface brightness caused by the magnetic field. The rotational period is slowing due to magnetic braking; it is one of the few magnetic stars to have its rotation period change directly measured. It was at one point suggested that σ Ori E could be further away and older than the other members of the cluster, from modelling its evolutionary age and size. σ Ori E has a faint companion about a third of an arc-second away. It is about 5 magnitudes fainter than the helium-rich primary, about magnitude 10–11 at K band infrared wavelengths. It is presumed to be a low mass star . ==σ Orionis IRS1==

The infrared source IRS1 is close to σ Ori A. It has been resolved to a pair of low mass objects, a proplyd, and a possible third object. The brighter object has an M1 spectral class, a mass around , and appears to be a relatively normal low mass star. The fainter object is very unusual, showing a diluted M7 or M8 absorption spectrum with emission lines of hydrogen and helium. The interpretation is that it is a brown dwarf embedded within a proplyd that is being photoevaporated by σ Ori A. X-ray emission from IRS1 suggests the presence of an accretion disc around a T Tauri star, but it is unclear how this can fit with the proplyd scenario. ==Dust wave==

In infrared images, a prominent arc is visible centred on σ Ori AB. It is about 50" away from the class O star, around 0.1 parsecs at its distance. It is directed towards IC434, the Horesehead Nebula, in line with the space motion of the star. The appearance is similar to a bowshock, but the type of radiation shows that it is not a bowshock. The observed infrared emission, peaking at around 45 microns, can be modelled by two approximately black-body components, one at 68K and one at 197 K. These are thought to be produced by two different sizes of dust grains. The material of the arc is theorised to be produced by photoevaporation from the molecular cloud around the Horsehead Nebula. The dust becomes decoupled from the gas that carried it away from the molecular cloud by radiation pressure from the hot stars at the centre of the σ Orionis cluster. The dust accumulates into a denser region that is heated and forms the visible infrared shape. The term "dust wave" is applied when the dust piles up but the gas is largely unaffected, as opposed to a "bow wave" where both dust and gas are stopped. Dust waves occur when the interstellar medium is sufficiently dense and the stellar wind sufficiently weak that the dust stand-off distance is larger than the stand-off distance of a bow shock. This would clearly be more likely for slow-moving stars, but slow-moving luminous stars may not have lifetimes long enough to produce a bow wave. Low luminosity late class O stars should commonly produce bow waves if this model is correct. Another study does however find that this feature is due σ Ori AB being a runaway star. Evidence for the runaway nature of the star are a different proper motion compared to the cluster, an infrared arc along the predicted velocity vector and a disparity in protoplanetary disk masses inside the cluster. The disks yet to encounter σ Ori AB have a higher disk mass, than those already encountered σ Ori AB. The disks already encountered have a reduced disk mass due to photoevaporation by the powerful radiation by σ Ori AB. This result needs confirmation by better constraining the proper motion of σ Ori AB. ==Distance==

The distance to σ Orionis and the cluster of stars around it has historically been uncertain. Hipparcos parallaxes were available for several presumed members, but with very high uncertainties for the σ Orionis components. Published distance estimates ranged from to . , and respectively. These have low statistical uncertainties although significant astrometric excess noise. No Gaia parallax has been published for the central AB component. Corresponding distances are , , and for components C, D, and E respectively. ==References==