When is the best time to observe 59 Aurigae?

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

Where is 59 Aurigae located in the sky?

59 Aurigae lies in the constellation Auriga at right ascension 06h 53m and declination +38° 52′.

What telescope do I need to split 59 Aurigae?

Splitting 59 Aurigae requires an aperture of roughly 60 mm or larger — the components are separated by about 22.2″ at magnitudes near 6.1. The companion is about 4.1 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

59 Aurigae — Double Star in Auriga

Magnitude 5.9–6.1^m DoubleStar Auriga (Aur) Visible

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1Physical Properties

Magnitude 6.12

Range 5.94 - 6.14

Period 3.7 hours

Variable Type Delta Scuti (Pulsating)

Spectral Type F2VDel Del

Star Color Yellow-white (B-V 0.37)

2Position & Identifiers

RA 06h 53m 01.5s

Dec +38° 52' 09.0"

Constellation Auriga (Aur)

HR 2539

HIP 33041

HD 50018

SAO 59571

Flamsteed 59 Aur

Variable ID OX Aur

Double Cat 5534

SIMBAD

3How easy to split?

Primary 6.1 mag Companion 10.2 mag Separation 22.2″

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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	Medium+	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 Nov – Jan (peak: Dec)

5Light Curve

6Multiple Star System Triple

Components 3 (triple)

Component IDs AB

Separation 22.2″

Companion Mag 10.2

Position Angle 224°

Star Colors A: Yellow-white B: Orange

Discoverer STF 974

Notes

AB fixed.

Separation over time

Measured 1782 → 2016 (234 y)

Separation drift 23.5" → 22.2" (-1.30")

Rate -0.0056" / y

PA drift 220° → 224° (+4°, +0.017°/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.