When is the best time to observe HIP 34489?

HIP 34489 is best observed from December through February, with peak visibility during January when it transits around midnight in the Northern Hemisphere.

Where is HIP 34489 located in the sky?

HIP 34489 lies in the constellation Canis Major at right ascension 07h 09m and declination -24° 03′.

What telescope do I need to split HIP 34489?

Splitting HIP 34489 requires an aperture of roughly 60 mm or larger — the components are separated by about 15.1″ at magnitudes near 6.7. The companion is about 4.4 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

HIP 34489 — Double Star in Canis Major

Magnitude 6.7^m DoubleStar Canis Major (CMa) Visible

Star Map + List + Plan Star Hop

Observe

1Physical Properties

Magnitude 6.65

Spectral Type B2V

Star Color Blue (B-V -0.19)

2Position & Identifiers

RA 07h 08m 49.3s

Dec -24° 02' 39.0"

Constellation Canis Major (CMa)

HR 2695

HIP 34489

HD 54669

SAO 173064

Variable ID Var?

SIMBAD

3How easy to split?

Primary 6.7 mag Companion 11.1 mag Separation 15.1″

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.	Hard+	Hard	V. hard+
150 mm Newton 150mm Newt.	Medium+	Medium	Medium
Celestron C8 (203 mm SCT) C8 203mm	Easy	Medium+	Medium

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 Dec – Feb (peak: Jan)

5Multiple Star System

Separation 15.1″

Companion Mag 11.1

Position Angle 286°

Star Colors A: Blue B: Yellow-white

Discoverer ARA2035

Separation over time

Measured 1922 → 2010 (88 y)

Separation drift 14.4" → 15.1" (+0.70")

Rate +0.0080" / y

PA drift 287° → 286° (-1°, -0.011°/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.