When is the best time to observe Lambda Coronae Australis?

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

Where is Lambda Coronae Australis located in the sky?

Lambda Coronae Australis lies in the constellation Corona Australis at right ascension 18h 44m and declination -38° 19′.

What telescope do I need to split Lambda Coronae Australis?

Splitting Lambda Coronae Australis requires an aperture of roughly 60 mm or larger — the components are separated by about 29.5″ at magnitudes near 5.1. The companion is about 4.9 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Lambda Coronae Australis — Double Star in Corona Australis

Magnitude 5.1^m DoubleStar Corona Australis (CrA) Visible

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Observe

1Physical Properties

Magnitude 5.13

Spectral Type A2Vn

Star Color White (B-V 0.09)

Distance 136 ly

2Position & Identifiers

RA 18h 43m 46.9s

Dec -38° 19' 25.0"

Constellation Corona Australis (CrA)

HR 7021

HIP 91875

HD 172777

SAO 210501

Bayer Lambda

SIMBAD

3How easy to split?

Primary 5.1 mag Companion 10.0 mag Separation 29.5″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Medium+	Medium	Hard+
150 mm Newton 150mm Newt.	Easy	Easy	Medium+
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 May – Jul (peak: Jun)

5Multiple Star System Triple C: optical

Components 3 (triple)

Component IDs AB

Separation 29.5″

Companion Mag 10.0

Position Angle 213°

Star Colors A: White B: Orange

Discoverer COO 227

Notes

Component B, K0.

Separation over time

Measured 1894 → 2016 (122 y)

Separation drift 25.0" → 29.5" (+4.50")

Rate +0.0369" / y

PA drift 215° → 213° (-2°, -0.016°/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.