When is the best time to observe 28 Aquilae?

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

Where is 28 Aquilae located in the sky?

28 Aquilae lies in the constellation Aquila at right ascension 19h 20m and declination +12° 22′.

What telescope do I need to split 28 Aquilae?

Splitting 28 Aquilae requires an aperture of roughly 60 mm or larger — the components are separated by about 60.7″ at magnitudes near 5.5. The companion is about 3.5 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

28 Aquilae — Double Star in Aquila

Magnitude 5.5^m DoubleStar Aquila (Aql) Visible

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Observe

1Physical Properties

Magnitude 5.53

Range 5.51 - 5.56

Period 3.6 hours

Variable Type Delta Scuti (Low Amplitude)

Spectral Type F0III giant

Star Color Yellow-white (B-V 0.26)

Distance 815 ly

2Position & Identifiers

RA 19h 19m 39.3s

Dec +12° 22' 29.0"

Constellation Aquila (Aql)

HR 7331

HIP 94982

HD 181333

SAO 104722

Flamsteed 28 Aql

Variable ID V1208 Aql

SIMBAD

3How easy to split?

Primary 5.5 mag Companion 9.0 mag Separation 60.7″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Easy	Medium+	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)

5Light Curve

6Multiple Star System Triple C: optical

Components 3 (triple)

Component IDs AB

Separation 60.7″

Companion Mag 9.0

Position Angle 175°

Star Colors A: Yellow-white B: Orange

Discoverer S 717

Separation over time

Measured 1822 → 2015 (193 y)

Separation drift 60.0" → 60.7" (+0.70")

Rate +0.0036" / y

PA drift 177° → 175° (-2°, -0.010°/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.

Eyepiece View

Telescope Eyepiece

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80x Dawes: 1.9″ TFOV: 0.6°

Seeing

Scale Realistic = true angular size

A: 5.5 · B: 9.0 · Sep: 60.7″ · PA: 175° · N up, E right

Resolved · Rayleigh: 2.3″ · Dawes: 1.9″ · Eff: 2.3″

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Size Comparison

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Compare Stars

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Spectral Classification

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Hertzsprung-Russell Diagram

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Stellar Lifecycle

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Blackbody Spectrum

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Stellar Absorption Spectrum

Simulated absorption spectrum based on spectral type. Hover over lines to identify elements.

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Stellar Fusion

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15Stellar Notes

Variable Star

Delta Sct 5.51 - 5.57V. Period analyses of new and existing data by Reed and Welch (1988, AJ, 95, 1510) indicate a | possible change in pulsational modes during the last several years, with fundamental period of 0.146d and possible | nonradial pulsations of 0.141, 0.183, and 0.091d.

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