When is the best time to observe V569 Monocerotis?

V569 Monocerotis is best observed from December through February, with peak visibility during January when it transits around midnight in the Northern Hemisphere.

Where is V569 Monocerotis located in the sky?

V569 Monocerotis lies in the constellation Monoceros at right ascension 07h 06m and declination -10° 40′.

What telescope do I need to split V569 Monocerotis?

Splitting V569 Monocerotis requires an aperture of roughly 60 mm or larger — the components are separated by about 38.0″ at magnitudes near 6.5. The companion is about 3.1 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

V569 Monocerotis — Double Star in Monoceros

Magnitude 6.4–6.5^m DoubleStar Monoceros (Mon) Visible

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Observe

1Physical Properties

Magnitude 6.49

Range 6.42 - 6.53

Period 6.4 hours

Variable Type Beta Cephei (Pulsating)

Spectral Type B0.5V+F5III

Star Color Blue (B-V -0.05)

2Position & Identifiers

RA 07h 05m 49.7s

Dec -10° 39' 40.0"

Constellation Monoceros (Mon)

HR 2670

HIP 34234

HD 53755

SAO 152363

Variable ID V569 Mon

Double Cat 5782

SIMBAD

3How easy to split?

Primary 6.5 mag Companion 9.6 mag Separation 38.0″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Medium+	Medium+	Medium
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 Dec – Feb (peak: Jan)

5Light Curve

6Multiple Star System Quadruple

Components 4 (quadruple)

Component IDs AC

Separation 38.0″

Companion Mag 9.6

Position Angle 296°

Star Colors A: Blue C: Yellow

Discoverer STF1019

Notes

Component B, 10.3v, F5III.

Separation over time

Measured 1830 → 2024 (194 y)

Separation drift 37.8" → 38.0" (+0.20")

Rate +0.0010" / y

PA drift 294° → 296° (+2°, +0.010°/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.