When is the best time to observe 24 Comae Berenices?

24 Comae Berenices is best observed from February through April, with peak visibility during March when it transits around midnight in the Northern Hemisphere.

Where is 24 Comae Berenices located in the sky?

24 Comae Berenices lies in the constellation Coma Berenices at right ascension 12h 35m and declination +18° 23′.

What telescope do I need to split 24 Comae Berenices?

Splitting 24 Comae Berenices requires an aperture of roughly 60 mm or larger — the components are separated by about 20.1″ at magnitudes near 5.0. Larger apertures and steady seeing help resolve the pair cleanly.

24 Comae Berenices — Double Star in Coma Berenices

Observable Double Star Excellent (71/100)

Sep: 20.1", Companion: mag 6.3

Magnitude 5.0^m DoubleStar Coma Berenices (Com) Visible

Star Map + List + Plan Star Hop

Observe

1Physical Properties

Magnitude 5.02

Spectral Type K2III giant

Star Color Red (B-V 1.15)

Distance 1,631 ly

2Position & Identifiers

RA 12h 35m 07.8s

Dec +18° 22' 37.0"

Constellation Coma Berenices (Com)

HR 4792

HIP 61418

HD 109511

SAO 100160

Flamsteed 24 Com

Double Cat 8600

SIMBAD

3How easy to split?

Primary 5.0 mag Companion 6.3 mag Separation 20.1″

Sign in and configure your equipment and default location to see a personalized row.

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

Set a location in User Settings to see visibility data.

Best season Feb – Apr (peak: Mar)

5Multiple Star System

Separation 20.1″

Companion Mag 6.3

Position Angle 271°

Star Colors A: Red B: Yellow-white

Discoverer STF1657

Notes

Binary with HR 4791.

Separation over time

Measured 1781 → 2023 (242 y)

Separation drift 18.4" → 20.1" (+1.70")

Rate +0.0070" / y

PA drift 274° → 271° (-3°, -0.012°/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.