When is the best time to observe HIP 61910?

HIP 61910 is best observed from February through April, with peak visibility during March when it transits around midnight in the Northern Hemisphere.

Where is HIP 61910 located in the sky?

HIP 61910 lies in the constellation Corvus at right ascension 12h 41m and declination -13° 01′.

What telescope do I need to split HIP 61910?

Splitting HIP 61910 requires an aperture of roughly 80 mm or larger — the components are separated by about 5.3″ at magnitudes near 6.0. Larger apertures and steady seeing help resolve the pair cleanly.

HIP 61910 — Double Star in Corvus

Observable Double Star Excellent (70/100)

Sep: 5.3", Companion: mag 5.9

Magnitude 5.1–5.2^m DoubleStar Corvus (Crv) Visible

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Observe

1Physical Properties

Magnitude 5.98

Range 5.11 - 5.25

Period 3.1 days

Variable Type Eclipsing Binary (Algol-type)

Spectral Type F5V

Star Color Yellow-white (B-V 0.42)

Distance 233 ly

2Position & Identifiers

RA 12h 41m 16.2s

Dec -13° 00' 54.0"

Constellation Corvus (Crv)

HR 4822

HIP 61910

HD 110318

SAO 157448

Double Cat 8627

SIMBAD

3How easy to split?

Primary 6.0 mag Companion 5.9 mag Separation 5.3″

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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 Feb – Apr (peak: Mar)

5Light Curve

6Multiple Star System Triple

Components 3 (triple)

Component IDs AB

Separation 5.3″

Companion Mag 5.9

Companion Sp F5V

Position Angle 314°

Star Colors A: Yellow-white B: Yellow-white

Discoverer STF1669

Notes

Binary with HR 4821. Colors for combined light. Mag. of blend, 5.27V. Component C, 10.5v at 59" optical.

Separation over time

Measured 1823 → 2020 (197 y)

Separation drift 6.9" → 5.3" (-1.60")

Rate -0.0081" / y

PA drift 299° → 314° (+15°, +0.076°/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.