Tycho Catalogue. UBV M UBV ALS Catalog of Galactic OB Stars. EUVE J The first Extreme Ultraviolet Explorer source catalog. Washington Double Star Catalog. WDS JA. SBC9 Eighth catalogue of the orbital elements of spectroscopic binary systems. CGO A catalogue of galactic O stars. The ionization of the low density interstellar medium by runaway stars.
GOS G A galactic O star catalog. HGAM A catalogue of Hgamma measures. SBC7 Seventh catalogue of the orbital elements of spectroscopic binary systems. The complete Einstein Observatory X-ray survey of the Orion nebula region. MSC - a catalogue of physical multiple stars. PMSC Aab. PMSC A. SOXS An X-ray survey of the young stellar population of the Lynds and iota Orionis regions. WEB Vitesses radiales. Radial velocities: The Wilson-Evans-Batten catalogue.
Flamsteed designation. New observational clues to understand macroturbulent broadening in massive O- and B-type stars. Rotational velocities in northern Galactic O- and early B-type stars revisited. The impact of other sources of line-broadening. Validation of the new Hipparcos reduction.
The Hipparcos Catalogue. Catalog of standard stars for the equinox and epoch Two curiously similar spectroscopic binaries. The O-type stars. The revision of the general catalogue of radial velocities. Catalog of individual radial velocities, 0hh, measured by astronomers of the Mount Wilson Observatory. The radial velocities of stars in the years to Radial velocities of helium stars. Ten stars whose radial velocities vary. SB9: The ninth catalogue of spectroscopic binary orbits. Zeeman measures of sharp lined early B stars.
Die Radialgeschwindigkeitskurve von iota Orionis. The orbit of iota Orionis. The spectroscopic binary iota Orionis. Orion variable. Spectral Classification. Spectral classification of OB stars in both hemispheres and the absolute magnitude calibration. Some spectroscopic characteristics of OB stars: an investigation of the space distribution of certain OB stars and the reference frame of the classification.
Line strengths for southerns OB stars. Observations with moderate dispersion. At magnitude 1. The star is so hot it lights up the surrounding interstellar gas, making its own reflection nebula labelled NGC Like the other two stars in Orion's belt it is very large, very hot, and very far away: an O9I blue supergiant with a surface temperature of 31, degrees K. It has two smaller, dimmer companions, making it a triple star system with a combined magnitude of 1. And the big, bad, far away blue stars keep coming with Kappa Orionis, named Saiph, from the Arabic for sword of the giant, even though it's in Orion's right foot.
It is a B0II bright giant with a magnitude of 2. Properly hanging from Orion's belt is Nair Al Saif, the bright one of the sword. It is a quadruple system, very similar to Mintaka: a B0III blue giant, and an O9III blue giant locked in a tight embrace, circling each other every 29 days, and two smaller, dimmer companions orbiting the massive binaries.
As with all the named star systems in Orion, Nair Al Saif is very far away, at a distance of about 1, light years, shining with a combined magnitude of 2. Upsilon Orionis is a small, dim little star near the bottom of the figure that is not little at all, but actually a very large O8V blue main sequence star with a mass 30 times greater than our Sun.
It appears so small and dim because it is very, very far away at a distance of about 3, light years, so despite having a searing surface temperature of 34, degrees K, and a luminosity at least 60, times greater than our Sun, it appears in our sky with the lowly magnitude of 4. Why the ancients named this faint star is a mystery. It carries the name Thabit, which R. Allen tells us is Arabic for the endurer, though he is unable to derive its origins.
To further confuse us, the star Pi3 Orionis has the same name, albeit differently spelled as Tabit. This star at least is a bit more visually impressive at magnitude 3. Significantly, this star is very different from all the other eleven named stars in Orion, which have all been massive, super hot blue stars many hundreds of light years away.
This star is an F6V yellow main sequence star with a nice, normal surface temperature of 6, degrees K, very similar to our Sun. What's more, this star is very close, only 26 light years away. Its proximity and Sun-like qualities mean a lot of telescopes have it in their sights, looking for planets and possible indications of life. At a distance of about 1, light years, its light reaches us with a magnitude of 3.
Meissa is the brightest of a star cluster named Collinder 69, and the combined energy of these stars has ionized a huge ring of interstellar gas around them called the Lambda Orionis Molecular Ring SH Not much to see in visible light, the nebula puts on quite a show in the infrared spectrum. Through the eyes of NASA's WISE infrared telescope red stars turn blue, blue stars turn red, and the surrounding emission nebula is a spectacular glowing green circle a staggering light years across.
At bottom left is the normally red Betelgeuse, in the centre is Meissa, and over on the right side is the normally blue Bellatrix. So far, eight planetary systems have been discovered within the boundaries of the Orion constellation, the closest of which is Gliese , only 39 light years away.
The star is an M4V red main sequence star with a surface temperature of only 3, degrees K, making it far too faint to see at magnitude There is one confirmed planet in the system with 0. An orbital radius of 2. Farther away at 66 light years is the Gliese system also designated BD , with two known planets so far. The dim, magnitude 9. Planet Gliese b is about the size of Neptune, in a day orbit, 42 million miles 67 million kms from the star.
Hatysa Luminosity Luminosity is the amount of energy that a star pumps out and its relative to the amount that our star, the Sun gives out.
The figure of 59, Hatysa estimated radius has been calculated as being The Sun's radius is ,km, therefore the star's radius is an estimated 7,, If you need the diameter of the star, you just need to multiple the radius by 2. However with the release of updated Hipparcos files, the radius is now calculated at being round The figure is derived at by using the formula from SDSS rather than peer reviewed papers. It has been known to produce widely incorrect figures.
Hatysa Iron Abundance is 0. The value comes from the Hipparcos Extended Catalog. Hatysa apparent magnitude is 2. Apparent Magnitude is also known as Visual Magnitude.
If you used the Parallax value, Hatysa absolute magnitude is Absolute Magnitude is the apparent magnitude of the star from a distance of 10 parsecs or This assumes that there is nothing in between the object and the viewer such as dust clouds.
To really compare the brightness of the star, it is best to use Absolute rather than Apparent Magnitude. Our own Sun is the brightest star and therefore has the lowest of all magnitudes, A faint star will have a high number. Using the original Hipparcos data that was released in , the parallax to the star was given as 2.
If you want that in miles, it is about 7,,,,, In , Hipparcos data was revised with a new parallax of 1. It should not be taken as though the star is moving closer or further away from Earth. It is purely that the distance was recalculated. Using the distance, the star is roughly ,, An Astronomical Unit is the distance between Earth and the Sun.
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