Alnitak 3

STScI, NASA




Larger image of
Constellation Orion.





Alnitak is the leftmost
star of the three bright
stars in Orion's belt.
(another image with
enhanced colors).

In the venerable Star Names: Their Lore and Meaning, Richard Hinckley Allen noted that its proper name, Alnitak (or Alnitah), is derived from the Arabic for Al Nitak meaning "The Belt" or "The Girdle" of Orion. Alnitak is the easternmost of the three stars of Orion's Belt, with Alnilam in the center and Mintaka in the west. All three were originally thought to be at a similar distance from Sol and (with Rigel, Saiph, and Meissa) probably formed at about the same time, around some 10 million years ago from the molecular clouds observed in Orion.

Davide De Martin
(Skyfactory),
Digitized Sky Survey,
ESA/ESO/NASA
FITS Liberator


Larger
composite image
of Orion's Belt.


Alnitak is the
leftmost star
of Orion's Belt
(more from
APOD).

In addition to wide binary companion Star B, Alnitak's primary also has a close stellar companion Ab, (USNO press release). However, the star (sometimes called "C") that has a separation of around 57.6" away is thought to be a optical companion. Alnitak lies in a region crowded with several dusty clouds of interstellar gas actively forming new stars, including the famous "Horsehead Nebula" to the south. The system is a member of the "Orion OB1 Association," where massive young objects with over 10 times the Sol's mass can be found in abundance (more on OB associations and stellar nurseries).

Zeta Orionis A or Aa

Alnitak Aa is a blue supergiant star of spectral and luminosity type O9.7 Ibe (with "peculiar" emission lines), where O-type stars are the hottest stars in the spectral sequence excluding white dwarfs. The star may have as much as 28 times Sol's mass (Hummel et al, 2000, in pdf), perhaps 20 times Sol's diameter (Remie and Lamers, 1982, page 87; as reported in Pasinetti-Fracassini et al, 2001), and around 100,000 times its bolometric luminosity, which is much greater than its visual luminosity of around 10,500 times Solar. The European Space Agency's astrometry satellite HIPPARCOS has measured Zeta Orionis Aab's distance from Earth to be around 820 light years, giving it an absolute visual magnitude of -5.25 (based on a HIPPARCOS Vmag= 1.74), somewhat under-luminous for stars of its class; however, these measurements may have been significantly affected by the presence of the recently discovered, dimmer close stellar companion Ab (described below). Even so, Alnitak Aa is the brightest O-type star in Earth's night sky (according to Professor Jim Kaler's excellent Stars' web page on Alnitak). Its 31,000-degree-Kelvin surface, however, radiates mostly ultraviolet wavelengths that are invisible to Human eyes.

NASA Observatorium



Alnitak Aa is hotter,
brighter, and bluer
than even Rigel or
Spica.



See a discussion of
"core helium burning"
as part of stellar
evolution and death.

Type-O supergiants show strong stellar winds that produce optical spectral emission lines and thermal radio and X-ray emissions. How these stars produce high-energy X-rays, however, is still subject to intense research because they lack significant magnetic fields and are not sufficiently hot despite their very high surface temperatures. Alnitak Aa seems to generate and maintain magnetic loops like Sol, which is difficult for astronomers to explain. Although O-type stars have inner convection zones in their core, they are believed to lack outer convection zones, which astronomers considered necessary to create the hot and energetic plasmas confined in magnetic loops. Convection zones are internal regions where most of the energy is transported by fluid motions from hotter regions to cooler ones. Without such zones located near a star's surface, astronomers are currently unable to explain how high-density knots of X-rays could exist. On the other hand, shock waves created in the turbulent stellar wind flow are an important part of current theories. Like all O stars, Alnitak Aa's X-rays may come from a wind that blows from its surface at nearly 2,000 km (1,200 miles) per second, which produces x-rays when blobs of gas in the wind crash violently into one another (Donati et al, 2002; Waldron and Cassinelli, 2001, and 2000 in pdf; and CXC press release, 10/18/2000).

Massive stars use their fuel quickly and do not live very long. Although Alnitak Aa may only be around six million years old, hydrogen fusion may already have ceased at its core. The star will eventually become a red supergiant somewhat like Betelgeuse and will probably explode as a supernova. Useful catalogue numbers and designations for the star include: Zet Ori A, 50 Ori A, HR 1948/9, HIP 26727, HD 37742, BD-02 1338, SAO 132444, STF 774 A, and ADS 4263 A.

Wayne R. Waldron, Joseph P. Cassinelli,
EIT, CXC, NASA


Larger x-ray image of Stars Aab and B.



The primary has a wide stellar
companion B that is currently
around 580 AUs (or 2.3") away
(more on x-ray emissions).

In a wide orbit around the primary is a 4th magnitude visual companion, a B-type giant star that is currently separated by about 2.3 arcseconds (USNO press release, 4/15/1998). The pair orbits each other with a period estimated around 1,500 years long. According to old calculations (from J. Hopmann in 1967) cited in the Sixth Catalog of Orbits of Visual Binaries, Star "B" is separated on average from the primary by around 680 AUs (a semi-major axis of a= 2.728" at a distance of 817 ly), with an estimated orbital period of 1,508.6 years. Their highly circular orbit (e= 0.07) is inclined 72.0° from the perspective of an observer from Earth.

Christian A. Hummel, NPOI, USNO
(Used with permission)


Larger, stacked three-color image of Stars
Aa and Ab (where colors indicate motion).


In addition to a blue-white, stellar companion
B in a wide orbit, Alnitak Aa has another,
closer stellar companion Ab (more).

In 1998, Star A was found to have a close stellar companion ("Ab") only around 11 AUs away (0.042" in February and March 1998 at a distance of 820 ly). The close companion is only two magnitudes fainter and would be easily visible to the naked eye from Earth if it was farther from its brighter neighbor. The relative motion of the inner stellar pair has been detected, which was "most likely due to their being gravitationaly bound with an orbital period of only a few years" (Hummel et al, 2000, in pdf; and USNO press release).

The distance from the star pair Aab where an Earth-type planet would be "comfortable" with liquid water is at least 300 AUs -- over seven times the orbital of Pluto in the Solar System. Given that the stars are only a few million years old, however, they are too probably young for any forming planets to have cooled off sufficiently to have much surface water instead of superheated steam. Astronomers would find it very difficult to detect an Earth-sized planet around this star using present methods.

Zeta Orionis Ab

As Star Ab has a high visual magnitude (around 4) and a presumably youthful age of a few million years shared with the primary, it may be a late O-type main sequence dwarf (Hummel et al, 2000, in pdf). Hence, it should have a much greater mass (e.g., 23 times Solar), diameter, and visual luminosity (over 1,300 times Solar) than Sol.

Zeta Orionis B

© AAO/ROE, photo by David Malin
(Used with permission)



Larger labelled image of Pleiades.



Alnitak B is a blue-white star
that is larger, brighter, and
hotter than Sirius A, like six
of the brightest stars of the
Pleiades Cluster at left.