When is the best time to observe HIP 92391?

HIP 92391 is best observed from May through July, with peak visibility during June when it transits around midnight in the Northern Hemisphere.

Where is HIP 92391 located in the sky?

HIP 92391 lies in the constellation Scutum at right ascension 18h 50m and declination -05° 55′.

What telescope do I need to split HIP 92391?

Splitting HIP 92391 requires an aperture of roughly 60 mm or larger — the components are separated by about 111.8″ at magnitudes near 6.0. Larger apertures and steady seeing help resolve the pair cleanly.

HIP 92391 — Double Star in Scutum

Observable Double Star Good (56/100)

Sep: 111.8", Companion: mag 8.2

Magnitude 6.0^m DoubleStar Scutum (Sct) Visible

Star Map + List + Plan Star Hop

Observe

1Physical Properties

Magnitude 5.99

Spectral Type K2Ib supergiant

Star Color Red (B-V 1.60)

2Position & Identifiers

RA 18h 49m 41.0s

Dec -05° 54' 46.0"

Constellation Scutum (Sct)

HR 7083

HIP 92391

HD 174208

Double Cat 11719

SIMBAD

3How easy to split?

Primary 6.0 mag Companion 8.2 mag Separation 111.8″

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 May – Jul (peak: Jun)

5Multiple Star System Triple

Components 3 (triple)

Component IDs AC

Separation 111.8″

Companion Mag 8.2

Position Angle 171°

Star Colors A: Red

Discoverer H 6 50

Notes

B, 12.5v at 23"; C, 8.14V, +1.05(B-V), +0.75(U-B), K0II-III.

Separation over time

Measured 1833 → 2016 (183 y)

Separation drift 99.0" → 111.8" (+12.80")

Rate +0.0699" / y

PA drift 169° → 171° (+2°, +0.011°/y)

Apparent motion is significant on a human timescale — worth revisiting in a decade.

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.