When is the best time to observe Delta Lyrae?

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

Where is Delta Lyrae located in the sky?

Delta Lyrae lies in the constellation Lyra at right ascension 18h 55m and declination +36° 54′.

What telescope do I need to split Delta Lyrae?

Splitting Delta Lyrae requires an aperture of roughly 60 mm or larger — the components are separated by about 86.3″ at magnitudes near 4.3. The companion is about 6.9 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Delta Lyrae — Double Star in Lyra

HIP 92791; Delta2 Lyrae; 12 Lyrae

Magnitude 4.2–4.3^m DoubleStar Lyra (Lyr) Visible

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1Physical Properties

Magnitude 4.30

Range 4.13 - 4.41

Variable Type Semi-Regular Variable

Spectral Type M4II bright giant

Star Color Red (B-V 1.68)

2Position & Identifiers

RA 18h 54m 30.2s

Dec +36° 53' 56.0"

Constellation Lyra (Lyr)

HR 7139

HIP 92791

HD 175588

SAO 67559

Bayer Delta2

Flamsteed 12 Lyr

Variable ID Del2 Lyr

Double Cat 11825

SIMBAD Wikipedia

3How easy to split?

Primary 4.3 mag Companion 11.2 mag Separation 86.3″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Hard+	Hard	V. hard+
150 mm Newton 150mm Newt.	Medium+	Medium	Hard+
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

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Best season May – Jul (peak: Jun)

5Multiple Star System Triple E,F,H,K: optical

Components 3 (triple)

Component IDs AB

Separation 86.3″

Companion Mag 11.2

Companion Sp B9/A0

Position Angle 349°

Star Colors A: Red B: Blue-white

Discoverer ES 2028

Separation over time

Measured 1923 → 2014 (91 y)

Separation drift 87.0" → 86.3" (-0.70")

Rate -0.0077" / y

PA drift 350° → 349° (-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.