When is the best time to observe 7 Leonis?

7 Leonis is best observed from January through March, with peak visibility during February when it transits around midnight in the Northern Hemisphere.

Where is 7 Leonis located in the sky?

7 Leonis lies in the constellation Leo at right ascension 09h 36m and declination +14° 23′.

What telescope do I need to split 7 Leonis?

Splitting 7 Leonis requires an aperture of roughly 60 mm or larger — the components are separated by about 41.0″ at magnitudes near 6.4. The companion is about 3.0 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

7 Leonis — Double Star in Leo

Magnitude 6.4^m DoubleStar Leo Visible

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Observe

1Physical Properties

Magnitude 6.36

Spectral Type A1V

Star Color White (B-V 0.01)

Distance 544 ly

2Position & Identifiers

RA 09h 35m 52.9s

Dec +14° 22' 47.0"

Constellation Leo

HR 3818

HIP 47096

HD 83023

SAO 98662

Flamsteed 7 Leo

Double Cat 7448

SIMBAD

3How easy to split?

Primary 6.4 mag Companion 9.4 mag Separation 41.0″

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Telescope	Bortle 3	Bortle 4	Bortle 5
80 mm refractor 80mm refr.	Medium+	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 Jan – Mar (peak: Feb)

5Multiple Star System Triple

Components 3 (triple)

Separation 41.0″

Companion Mag 9.4

Position Angle 90°

Star Colors A: White B: Yellow

Discoverer H 5 58

Notes

CPM. Companion F8V. Discordant magnitudes and colors: Nicolet: A = 7.86V, -0.10(B-V), -0.43(U-B); B = 9.07V, | +0.55(B-V), +0.01(U-B). USNO Photoelectric Catalogue: A = 6.36V, +0.01(B-V), +0.03(U-B); B = 9.51V, +0.50(B-V), | +0.03(U-B). Component A suspected occultation double.

Separation over time

Measured 1782 → 2014 (232 y)

Separation drift 42.4" → 41.0" (-1.40")

Rate -0.0060" / y

PA drift 81° → 90° (+9°, +0.039°/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.