When is the best time to observe 14 Aurigae?

14 Aurigae is best observed from November through January, with peak visibility during December when it transits around midnight in the Northern Hemisphere.

Where is 14 Aurigae located in the sky?

14 Aurigae lies in the constellation Auriga at right ascension 05h 15m and declination +32° 41′.

What telescope do I need to split 14 Aurigae?

Splitting 14 Aurigae requires an aperture of roughly 60 mm or larger — the components are separated by about 14.3″ at magnitudes near 5.0. Larger apertures and steady seeing help resolve the pair cleanly.

14 Aurigae — Double Star in Auriga

Observable Double Star Excellent (61/100)

Sep: 14.3", Companion: mag 7.3

Magnitude 4.9–5.1^m DoubleStar Auriga (Aur) Visible

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1Physical Properties

Magnitude 5.02

Range 4.95 - 5.08

Period 2.1 hours

Variable Type Delta Scuti (Low Amplitude)

Spectral Type A9IVDel Del subgiant

Star Color Yellow-white (B-V 0.23)

Distance 466 ly

2Position & Identifiers

RA 05h 15m 24.4s

Dec +32° 41' 16.0"

Constellation Auriga (Aur)

HR 1706

HIP 24504

HD 33959

SAO 57799

Flamsteed 14 Aur

Variable ID KW Aur

Double Cat 3824

SIMBAD

3How easy to split?

Primary 5.0 mag Companion 7.3 mag Separation 14.3″

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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

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Best season Nov – Jan (peak: Dec)

5Light Curve

6Multiple Star System Quadruple optical

Components 4 (quadruple)

Component IDs AC

Separation 14.3″

Companion Mag 7.3

Companion Sp F2V

Position Angle 225°

Star Colors A: Yellow-white C: Yellow-white

Discoverer STF 653

Notes

AC binary. B, 11v F4V at 13" optical.

Separation over time

Measured 1780 → 2019 (239 y)

Separation drift 16.1" → 14.3" (-1.80")

Rate -0.0075" / y

PA drift 232° → 225° (-7°, -0.029°/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.