When is the best time to observe Eta Canis Minoris?

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

Where is Eta Canis Minoris located in the sky?

Eta Canis Minoris lies in the constellation Canis Minor at right ascension 07h 28m and declination +06° 57′.

What telescope do I need to split Eta Canis Minoris?

Splitting Eta Canis Minoris requires an aperture of roughly 250 mm or larger — the components are separated by about 4.3″ at magnitudes near 5.2. The companion is about 5.8 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Eta Canis Minoris — Double Star in Canis Minor

Magnitude 5.2^m DoubleStar Canis Minor (CMi) Visible

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Observe

1Physical Properties

Magnitude 5.25

Spectral Type F0III giant

Star Color Yellow-white (B-V 0.22)

Distance 326 ly

2Position & Identifiers

RA 07h 28m 02.1s

Dec +06° 56' 31.0"

Constellation Canis Minor (CMi)

HR 2851

HIP 36265

HD 58923

SAO 115477

Bayer Eta

Flamsteed 5 CMi

Double Cat 6101

SIMBAD

3How easy to split?

Primary 5.3 mag Companion 11.1 mag Separation 4.3″

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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	Hard+	Hard+	Hard+

Easy Medium Hard Very hard Impossible

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

To reach "Medium" at Bortle 3, you'd need at least a 250 mm reflector.

4Visibility

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Best season Dec – Feb (peak: Jan)

5Multiple Star System

Separation 4.3″

Companion Mag 11.1

Position Angle 28°

Star Colors A: Yellow-white

Discoverer BU 21

Notes

CPM.

Separation over time

Measured 1872 → 2016 (144 y)

Separation drift 5.0" → 4.3" (-0.70")

Rate -0.0049" / y

PA drift 30° → 28° (-2°, -0.014°/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.