When is the best time to observe SV Crateris?

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

Where is SV Crateris located in the sky?

SV Crateris lies in the constellation Crater at right ascension 11h 17m and declination -07° 08′.

What telescope do I need to split SV Crateris?

Splitting SV Crateris requires an aperture of roughly 60 mm or larger — the components are separated by about 53.2″ at magnitudes near 6.1. Larger apertures and steady seeing help resolve the pair cleanly.

SV Crateris — Double Star in Crater

DoubleStar Crater (Crt) Visible

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Observe

1Physical Properties

Magnitude 6.14

Variable Type Alpha2 CVn (Magnetic Rotating)

Spectral Type A8IVpeSrCrSi

Star Color Yellow-white (B-V 0.20)

Distance 815 ly

2Position & Identifiers

RA 11h 16m 58.2s

Dec -07° 08' 05.0"

Constellation Crater (Crt)

HR 4369

HIP 55106

HD 98088

Variable ID SV Crt

Double Cat 8115

SIMBAD

3How easy to split?

Primary 6.1 mag Companion 8.2 mag Separation 53.2″

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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 Feb – Apr (peak: Mar)

5Multiple Star System Triple

Components 3 (triple)

Component IDs AC

Separation 53.2″

Companion Mag 8.2

Position Angle 99°

Star Colors A: Yellow-white C: Orange

Discoverer BU 600

Notes

AB CPM. B, 11.5v at 1". C, optical.

Separation over time

Measured 1823 → 2017 (194 y)

Separation drift 67.1" → 53.2" (-13.90")

Rate -0.0716" / y

PA drift 98° → 99° (+1°, +0.005°/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.

Eyepiece View

Telescope Eyepiece

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80x Dawes: 1.9″ TFOV: 0.6°

Seeing

Scale Realistic = true angular size

A: 6.1 · B: 8.2 · Sep: 53.2″ · PA: 99° · N up, E left

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

Explore

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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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Read: The Hertzsprung-Russell Diagram — Reading Stars Like a Map

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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

Discover

14Stellar Notes

Variable Star

ADS 8115A, brighter component of the SB system, Alpha CV 6.32 - 6.35B, 5.90513d, two unequal max. Same rotation and | magnetic per., related var. EuII and SrII emission.

Spectroscopic Binary

ADS 8115A, 5.90513d, K 74.7k/s, V0 -8.1k/s, msin3i 1.73, asini 5.98. Apsidal per. about 700 yrs. Rare example of | an Ap star member of a close binary.

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