When is the best time to observe 6 Cassiopeiae?

6 Cassiopeiae is best observed from August through October, with peak visibility during September when it transits around midnight in the Northern Hemisphere.

Where is 6 Cassiopeiae located in the sky?

6 Cassiopeiae lies in the constellation Cassiopeia at right ascension 23h 49m and declination +62° 13′.

What telescope do I need to split 6 Cassiopeiae?

Splitting 6 Cassiopeiae requires an aperture of roughly 150 mm or larger — the components are separated by about 1.5″ at magnitudes near 5.4. Larger apertures and steady seeing help resolve the pair cleanly.

6 Cassiopeiae — Double Star in Cassiopeia

Observable Double Star Fair (26/100)

Sep: 1.5", Companion: mag 8.0

Magnitude 5.3–5.5^m DoubleStar Cassiopeia (Cas) Visible

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Observe

1Physical Properties

Magnitude 5.43

Range 5.34 - 5.45

Period 37 days

Variable Type ACYG

Spectral Type A3Ia supergiant

Star Color Yellow (B-V 0.67)

Distance 3,262 ly

2Position & Identifiers

RA 23h 48m 50.2s

Dec +62° 12' 52.0"

Constellation Cassiopeia (Cas)

HR 9018

HIP 117447

HD 223385

SAO 20869

Flamsteed 6 Cas

Variable ID V566 Cas

Double Cat 17022

SIMBAD

3How easy to split?

Primary 5.4 mag Companion 8.0 mag Separation 1.5″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	V. hard+	V. hard+	V. hard+
150 mm Newton 150mm Newt.	Hard+	Hard+	Hard+
Celestron C8 (203 mm SCT) C8 203mm	Medium	Medium	Medium

Easy Medium Hard Very hard Impossible

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

4Visibility

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Best season Aug – Oct (peak: Sep)

5Light Curve

6Multiple Star System Triple G: optical

Components 3 (triple)

Component IDs AB

Separation 1.5″

Companion Mag 8.0

Position Angle 194°

Star Colors A: Yellow B: Orange

Discoverer STT 508

Notes

AB binary. B is cA0.

Separation over time

Measured 1843 → 2015 (172 y)

Separation drift 1.1" → 1.5" (+0.40")

Rate +0.0023" / y

PA drift 195° → 194° (-1°, -0.006°/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.