When is the best time to observe Denebola?

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

Where is Denebola located in the sky?

Denebola lies in the constellation Leo at right ascension 11h 49m and declination +14° 34′.

What telescope do I need to split Denebola?

Splitting Denebola requires an aperture of roughly 60 mm or larger — the components are separated by about 235.8″ at magnitudes near 2.1. The companion is about 6.3 magnitudes fainter, so glare from the primary — not separation — sets the minimum aperture. Larger apertures and steady seeing help resolve the pair cleanly.

Denebola — Double Star in Leo

HIP 57632; Beta Leonis; 94 Leonis

DoubleStar Leo Visible

Star Map + List + Plan

About Denebola

Description

Denebola is a white main-sequence star of spectral type A3V at magnitude 2.14, the second brightest star in Leo. Located about 36 light-years from Earth, it has a luminosity of roughly 15 times solar. Denebola marks the tail of the Lion and is one of the nearest A-type stars to the Sun. It has an infrared excess suggesting a debris disk.

Observing Tips

Denebola marks the eastern end (tail) of Leo, forming the apex of the triangle of stars (with Zosma and Chertan) that makes up the Lion's hindquarter. It is easy to find as the bright star east of Regulus and the Sickle. Denebola is also part of the Spring Triangle with Arcturus and Spica. Best observed March through June.

History

The name Denebola comes from the Arabic 'dhanab al-asad,' meaning 'the tail of the lion.' Like Vega and Fomalhaut, Denebola has a debris disk detected in infrared, making it a candidate for harboring a planetary system. It is a member of the IC 2391 supercluster, a group of young stars with similar ages.

Fun Facts

Denebola is the 'tail tip' of the Spring Triangle asterism, a large triangle also including Arcturus and Spica visible on spring evenings. Its debris disk suggests planets may orbit it, but none have been confirmed. At only 36 light-years, it is one of the nearest A-type stars to the Sun.

Observe

1Physical Properties

Magnitude 2.14

Variable Type Delta Scuti (Pulsating)

Spectral Type A3V

Star Color White (B-V 0.09)

Distance 36 ly

2Position & Identifiers

RA 11h 49m 03.6s

Dec +14° 34' 19.0"

Constellation Leo

HR 4534

HIP 57632

HD 102647

Bayer Beta

Flamsteed 94 Leo

Variable ID Bet Leo

Double Cat 8314

SIMBAD Wikipedia

3How easy to split?

Primary 2.1 mag Companion 8.5 mag Separation 235.8″

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

Set a location in User Settings to see visibility data.

Best season Feb – Apr (peak: Mar)

5Multiple Star System Quadruple C: optical

Components 4 (quadruple)

Component IDs AD

Separation 235.8″

Companion Mag 8.5

Position Angle 194°

Star Colors A: White

Discoverer BU 604

Notes

B, 15.7v at 40" physical; C, 13v at 80" optical.

Separation over time

Measured 1833 → 2022 (189 y)

Separation drift 298.0" → 235.8" (-62.20")

Rate -0.3291" / y

PA drift 204° → 194° (-10°, -0.053°/y)

Apparent motion is significant on a human timescale — worth revisiting in a decade.

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.