When is the best time to observe V826 Herculis?

V826 Herculis is best observed from May through July, with peak visibility during June when it transits around midnight in the Northern Hemisphere.

Where is V826 Herculis located in the sky?

V826 Herculis lies in the constellation Hercules at right ascension 17h 46m and declination +39° 19′.

What telescope do I need to split V826 Herculis?

Splitting V826 Herculis requires an aperture of roughly 80 mm or larger — the components are separated by about 7.9″ at magnitudes near 6.7. The companion is about 3.3 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

V826 Herculis — Double Star in Hercules

Magnitude 6.7^m DoubleStar Hercules (Her) Visible

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Observe

1Physical Properties

Magnitude 6.68

Spectral Type K3III+F7V giant

Star Color Red (B-V 1.39)

2Position & Identifiers

RA 17h 45m 58.5s

Dec +39° 19' 21.0"

Constellation Hercules (Her)

HR 6626

HIP 86946

HD 161832

SAO 66317

Variable ID V826 Her

Double Cat 10782

SIMBAD

3How easy to split?

Primary 6.7 mag Companion 10.0 mag Separation 7.9″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Medium+	Medium	Hard+
150 mm Newton 150mm Newt.	Easy	Easy	Medium+
Celestron C8 (203 mm SCT) 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 May – Jul (peak: Jun)

5Multiple Star System Triple C: optical

Components 3 (triple)

Component IDs AB

Separation 7.9″

Companion Mag 10.0

Position Angle 349°

Star Colors A: Red

Discoverer STF2224

Notes

Component B, 9.70V, +0.75(B-V), +0.19(U-B), F5V, binary. Component C mag. diff 5.36v at 70" from A.

Separation over time

Measured 1831 → 2016 (185 y)

Separation drift 7.5" → 7.9" (+0.40")

Rate +0.0022" / y

PA drift 352° → 349° (-3°, -0.016°/y)

Essentially fixed on human timescales — the same view your grandchildren will see.

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.