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Nair al Saif — Double Star in Orion

HIP 26241; Iota Orionis; 44 Orionis

Observable Double Star Good (58/100)

Sep: 11.2", Companion: mag 7.7

Magnitude 2.8m DoubleStar Orion (Ori) Visible
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About Nair al Saif

Description

Nair al Saif is a hot blue star of spectral type O9III at magnitude 2.77 in Orion. Located about 1,300 light-years from Earth, it has a luminosity of roughly 68,000 times solar and is one of the few O-type stars visible to the naked eye. It lies at the tip of Orion's Sword, below the Great Orion Nebula.

Observing Tips

Nair al Saif is the bottom star of Orion's Sword, below the Orion Nebula (M42). It is a blue-white star marking the sword's tip. The surrounding area is rich in nebulosity visible in photographs. Best observed December through March.

History

The name Nair al Saif comes from the Arabic 'nayyir al-sayf,' meaning 'the bright one of the sword.' As an O-type star, it is one of the hottest and most massive stars visible to the naked eye. It illuminates the nearby nebula NGC 1980.

Fun Facts

Iota Ori is a trapezium-like multiple star system similar to the famous Trapezium in M42. Its extreme luminosity and temperature contribute to ionizing the surrounding interstellar medium in the Orion OB1 association.

Observe

1Physical Properties

Magnitude 2.77
Range 2.76 - 2.79
Period 29.1 days
Variable Type Luminous Blue Variable
Spectral Type O9.5III giant
Star Color Blue (B-V -0.24)
Distance 1,439 ly

2Position & Identifiers

RA 05h 35m 26.0s
Dec -05° 54' 36.0"
Constellation Orion (Ori)
HR 1899
HIP 26241
HD 37043
SAO 132323
Bayer Iota
Flamsteed 44 Ori
Double Cat 4193

3How easy to split?

Primary 2.8 mag Companion 7.7 mag Separation 11.2″
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Telescope Bortle 3 Bortle 4 Bortle 5
80mm refr. Medium+ Medium+ Medium+
150mm Newt. Easy Easy Easy
C8 203mm Easy Easy Easy
Easy Medium Hard Very hard Impossible

Bortle 3 = rural · 4 = outer suburbs · 5 = suburbs

4Visibility

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Best season Nov – Jan (peak: Dec)

5Light Curve

6Multiple Star System Triple optical

Components 3 (triple)
Component IDs AB
Separation 11.2″
Companion Mag 7.7
Companion Sp B2V
Position Angle 141°
Star Colors A: Blue B: Blue
Discoverer STF 752
AB fixed. B is B7IV; vsini 50k/s.

Separation over time

Measured 1779 → 2023 (244 y)
Separation drift 12.5" → 11.2" (-1.30")
Rate -0.0053" / y
PA drift 134° → 141° (+7°, +0.029°/y)

Slow change over generations — observable in lifetime comparisons.

Measured from the WDS observational archive. No orbital solution has been derived — most likely the period is too long to fit an orbit to the available measurement arc.

Eyepiece View

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80x Dawes: 1.9″ TFOV: 0.6°
Realistic = true angular size
N E 141°

A: 2.8 · B: 7.7 · Sep: 11.2″ · PA: 141° · N up, E right

Resolved · Rayleigh: 2.3″ · Dawes: 1.9″ · Eff: 2.3″

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Size Comparison

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Spectral Classification

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Hertzsprung-Russell Diagram

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Stellar Lifecycle

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Blackbody Spectrum

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Stellar Absorption Spectrum

Simulated absorption spectrum based on spectral type. Hover over lines to identify elements.

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Stellar Fusion

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16Stellar Notes

Component B is NSV 2334, 7.4V.
ADS 4193A, 29.1351d, K 115.2k/s, V0 +26.6k/s, msin3i 15.7, asini 30.0.
Color excess E(B-V) = +0.07.
Iota Ori cluster; Ori OB1c4; sword of Orion; HII region.
Enhanced ultraviolet emission. Helium weak. Interstellar Lyman alpha absorption observed by AEROBEE rocket. | Iota Ori B is a helium weak star. Helium deficient by factor of 10 relative to standard stars. P and Ga enormously | enhanced. uv 1240 absorption strong; weak 1548.
0.005".
ADS 4193A, mass ejection vel. up to 1600k/s. ADS 4193B, +16k/s.
Nair al Saif; Hatysa in Becvar.
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Light Travel Time Machine

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Relativistic Travel

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