When is the best time to observe HIP 106886?

HIP 106886 is best observed from July through September, with peak visibility during August when it transits around midnight in the Northern Hemisphere.

Where is HIP 106886 located in the sky?

HIP 106886 lies in the constellation Cepheus at right ascension 21h 39m and declination +57° 29′.

What telescope do I need to split HIP 106886?

Splitting HIP 106886 requires an aperture of roughly 60 mm or larger — the components are separated by about 11.9″ at magnitudes near 5.6. Larger apertures and steady seeing help resolve the pair cleanly.

HIP 106886 — Double Star in Cepheus

Observable Double Star Excellent (69/100)

Sep: 11.9", Companion: mag 7.5

DoubleStar Cepheus (Cep) Visible

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Observe

1Physical Properties

Magnitude 5.62

Spectral Type O6.5V((f))

Star Color Yellow-white (B-V 0.21)

2Position & Identifiers

RA 21h 38m 57.6s

Dec +57° 29' 21.0"

Constellation Cepheus (Cep)

HR 8281

HIP 106886

HD 206267

Double Cat 15184

SIMBAD

3How easy to split?

Primary 5.6 mag Companion 7.5 mag Separation 11.9″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Easy	Easy	Easy
150 mm Newton 150mm Newt.	Easy	Easy	Easy
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 Jul – Sep (peak: Aug)

5Multiple Star System Quintuple C,D: optical

Components 5 (quintuple)

Component IDs AC

Separation 11.9″

Companion Mag 7.5

Companion Sp O9V

Position Angle 120°

Star Colors A: Yellow-white C: Blue

Discoverer STF2816

Notes

AC fixed. C, 8.05V, +0.23(B-V), -0.68(U-B), B1.5V at 12", vsini 80k/s. AD also fixed. D, 8.03V, +0.20(B-V), -0.72(U-B), | B2IV at 20", vsini 270k/s. In earlier sources C is brighter than D.

Separation over time

Measured 1782 → 2023 (241 y)

Separation drift 11.6" → 11.9" (+0.30")

Rate +0.0012" / y

PA drift 125° → 120° (-5°, -0.021°/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.