When is the best time to observe Aladfar?

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

Where is Aladfar located in the sky?

Aladfar lies in the constellation Lyra at right ascension 19h 14m and declination +39° 09′.

What telescope do I need to split Aladfar?

Splitting Aladfar requires an aperture of roughly 60 mm or larger — the components are separated by about 28.4″ at magnitudes near 4.4. The companion is about 4.2 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Aladfar — Double Star in Lyra

HIP 94481; Eta Lyrae; 20 Lyrae

Observable Double Star Good (53/100)

Sep: 28.4", Companion: mag 8.6

Magnitude 4.4^m DoubleStar Lyra (Lyr) Visible

Star Map + List + Plan

Observe

1Physical Properties

Magnitude 4.39

Spectral Type B2.5IV subgiant

Star Color Blue-white (B-V -0.15)

Distance 1,631 ly

2Position & Identifiers

RA 19h 13m 45.5s

Dec +39° 08' 46.0"

Constellation Lyra (Lyr)

HR 7298

HIP 94481

HD 180163

SAO 68010

Bayer Eta

Flamsteed 20 Lyr

Double Cat 12197

SIMBAD Wikipedia

3How easy to split?

Primary 4.4 mag Companion 8.6 mag Separation 28.4″

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 Jun – Aug (peak: Jul)

5Multiple Star System Triple C: optical

Components 3 (triple)

Component IDs AB

Separation 28.4″

Companion Mag 8.6

Companion Sp A0

Position Angle 81°

Star Colors A: Blue-white B: Blue-white

Discoverer STF2487

Notes

B is A0, optical.

Separation over time

Measured 1777 → 2017 (240 y)

Separation drift 26.0" → 28.4" (+2.40")

Rate +0.0100" / y

PA drift 90° → 81° (-9°, -0.037°/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.