When is the best time to observe HIP 107930?

HIP 107930 is best observed from July through September, with peak visibility during August when it transits around midnight in the Northern Hemisphere.

Where is HIP 107930 located in the sky?

HIP 107930 lies in the constellation Cepheus at right ascension 21h 52m and declination +55° 48′.

What telescope do I need to split HIP 107930?

Splitting HIP 107930 requires an aperture of roughly 60 mm or larger — the components are separated by about 17.6″ at magnitudes near 5.7. Larger apertures and steady seeing help resolve the pair cleanly.

HIP 107930 — Double Star in Cepheus

Observable Double Star Excellent (67/100)

Sep: 17.6", Companion: mag 6.4

Magnitude 5.7^m DoubleStar Cepheus (Cep) Visible

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Observe

1Physical Properties

Magnitude 5.71

Variable Type Beta Cephei (Pulsating)

Spectral Type B6IV-V subgiant

Star Color Blue-white (B-V -0.13)

Distance 652 ly

2Position & Identifiers

RA 21h 52m 01.0s

Dec +55° 47' 49.0"

Constellation Cepheus (Cep)

HR 8357

HIP 107930

HD 208095

SAO 33819

Double Cat 15405

SIMBAD

3How easy to split?

Primary 5.7 mag Companion 6.4 mag Separation 17.6″

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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 Triple B: optical

Components 3 (triple)

Component IDs AB

Separation 17.6″

Companion Mag 6.4

Position Angle 197°

Star Colors A: Blue-white B: Blue-white

Discoverer STF2840

Notes

AB CPM. B is A1p Sr Si, vsini 60k/s. C, 13.2v at 55".

Separation over time

Measured 1782 → 2024 (242 y)

Separation drift 21.1" → 17.6" (-3.50")

Rate -0.0145" / y

PA drift 192° → 197° (+5°, +0.021°/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.