When is the best time to observe WZ Cassiopeiae?

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

Where is WZ Cassiopeiae located in the sky?

WZ Cassiopeiae lies in the constellation Cassiopeia at right ascension 00h 01m and declination +60° 21′.

What telescope do I need to split WZ Cassiopeiae?

Splitting WZ Cassiopeiae requires an aperture of roughly 60 mm or larger — the components are separated by about 57.8″ at magnitudes near 6.9. Larger apertures and steady seeing help resolve the pair cleanly.

WZ Cassiopeiae — Double Star in Cassiopeia

Observable Variable Star

Range: 6.8 - 7.7, Period: 186.0d, Type: SRB

Carbon Star

Beautiful color contrast with blue companion; Carbon star

Read: Carbon Stars — The Reddest Stars You'll Ever See

DoubleStar Cassiopeia (Cas) Visible

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Observe

1Physical Properties

Magnitude 6.90

Range 6.8 - 7.7

Period 186 days

Variable Type Semi-Regular Variable (Late-type Giant)

Spectral Type C

Star Color Deep ruby red (B-V 3.00)

2Position & Identifiers

RA 00h 01m 16.0s

Dec +60° 21' 19.0"

Constellation Cassiopeia (Cas)

HR 9114

HIP 99

HD 224855

Variable ID WZ Cas

SIMBAD

3How easy to split?

Primary 6.9 mag Companion 8.3 mag Separation 57.8″

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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 Aug – Oct (peak: Sep)

5Light Curve

6Comparison Stars for WZ Cas (6.8–7.7)

Nearby stable stars for estimating brightness (AAVSO)

Loading comparison stars…

7Multiple Star System

Separation 57.8″

Companion Mag 8.3

Companion Sp G5

Position Angle 89°

Star Colors A: Red B: Orange

Discoverer STTA254

Separation over time

Measured 1874 → 2019 (145 y)

Separation drift 58.9" → 57.8" (-1.10")

Rate -0.0076" / y

PA drift 90° → 89° (-1°, -0.007°/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.