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Gamma Lupi — Double Star in Lupus

Magnitude 2.8m DoubleStar Lupus (Lup) Visible
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About Gamma Lup

Description

Gamma Lupi is a blue subgiant of spectral type B2IV at magnitude 2.78, the third brightest star in Lupus. Located about 420 light-years from Earth, it has a luminosity of roughly 8,500 times solar. It is a spectroscopic binary with a period of about 2.8 days.

Observing Tips

Gamma Lup lies in the body of Lupus, between Alpha Lup and the stars of Centaurus. It is a blue-white star in a rich part of the southern Milky Way. Only visible from the southern hemisphere and low northern latitudes. Best observed May through July.

History

Gamma Lupi has no traditional proper name. Like the other bright stars of Lupus, it is a member of the Scorpius-Centaurus OB association and formed relatively recently in astronomical terms.

Fun Facts

Gamma Lup's short-period spectroscopic binary means its two components orbit incredibly close together — completing a full orbit in less than 3 days, far faster than Mercury orbits the Sun.

Observe

1Physical Properties

Magnitude 2.78
Spectral Type B2 IV subgiant
Star Color Blue (B-V -0.20)
Distance 408 ly

2Position & Identifiers

RA 15h 35m 08.5s
Dec -41° 10' 01.0"
Constellation Lupus (Lup)
HR 5776
HIP 76297
HD 138690
SAO 225938
Bayer Gamma

3How easy to split?

Primary 2.8 mag Companion 3.5 mag Separation 0.8″
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Telescope Bortle 3 Bortle 4 Bortle 5
80mm refr. V. hard V. hard V. hard
150mm Newt. Hard Hard Hard
C8 203mm Hard Hard Hard
Easy Medium Hard Very hard Impossible

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

To reach "Medium" at Bortle 3, you'd need at least a 270 mm reflector.

4Visibility

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Best season Apr – Jun (peak: May)

5Multiple Star System D: optical

Separation 0.8″
Companion Mag 3.5
Position Angle 275°
Star Colors A: Blue B: Blue-white
Discoverer HJ 4786
3.5 B2IV-V, 3.6 B2IV-V, 147y, a = 0.59". Combined mag., colors.

Separation over time

Period: 201.4 y Eccentricity: 0.630 Now: 0.83", PA 95° -0.00" in 5 years
0.00" 0.24" 0.48" 0.72" 0.96" 2025 2030 2035 2040 2045 0.83"

Apparent separation over time, computed from ORB6 orbital elements. Steep curves indicate fast-changing pairs — catch them while they're splittable.

Eyepiece View

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80x Dawes: 1.9″ TFOV: 0.6°
Realistic = true angular size
N E 275°

A: 2.8 · B: 3.5 · Sep: 0.8″ · PA: 275° · N up, E right

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

Explore

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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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15Stellar Notes

Probable member of Sco-Cen cluster; upper Cen group of Sco-Cen assoc.
Spectra obtained in March 1987 at Vainu Bappu Obs. showed H alpha profiles with emission peaks. The star may be in | transition from B to Be type.
Expanding circumstellar shell.
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Light Travel Time Machine

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Relativistic Travel

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