When is the best time to observe V1030 Orionis?

V1030 Orionis is best observed from November through January, with peak visibility during December when it transits around midnight in the Northern Hemisphere.

Where is V1030 Orionis located in the sky?

V1030 Orionis lies in the constellation Orion at right ascension 05h 39m and declination -02° 36′.

What telescope do I need to split V1030 Orionis?

Splitting V1030 Orionis requires an aperture of roughly 60 mm or larger — the components are separated by about 52.9″ at magnitudes near 6.7. Larger apertures and steady seeing help resolve the pair cleanly.

V1030 Orionis — Double Star in Orion

Magnitude 6.6–6.8^m DoubleStar Orion (Ori) Visible

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Observe

1Physical Properties

Magnitude 6.65

Range 6.61 - 6.77

Period 28.6 hours

Variable Type SX Arietis (Magnetic Rotating)

Spectral Type B2Vp

Star Color Blue (B-V -0.19)

Distance 466 ly

2Position & Identifiers

RA 05h 38m 47.1s

Dec -02° 35' 39.0"

Constellation Orion (Ori)

HR 1932

HIP 26551

HD 37479

SAO 132408

Variable ID V1030 Ori

Double Cat 4241

SIMBAD

3How easy to split?

Primary 6.7 mag Companion 8.8 mag Separation 52.9″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Easy	Easy	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 Nov – Jan (peak: Dec)

5Light Curve

6Multiple Star System Quintuple

Components 5 (quintuple)

Component IDs AB

Separation 52.9″

Companion Mag 8.8

Companion Sp A

Position Angle 241°

Star Colors A: Blue B: Yellow-white

Discoverer STF 762

Notes

See HR 1931. Speculation that component E may be captured star older than the other components.

Separation over time

Measured 1831 → 2019 (188 y)

Separation drift 52.3" → 52.9" (+0.60")

Rate +0.0032" / y

PA drift 240° → 241° (+1°, +0.005°/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.