The celestial equator is the extension of Earth's equatorial plane onto the celestial sphere, so the two are coplanar; the approximately 23.44° angle is between the celestial equator and the ecliptic, not between the two equators. Stellar right ascension and declination depend on reference frame, epoch (such as J2000.0), precession, and proper motion; they are not perfectly constant. A figure-eight analemma is plotted from the Sun's position at the same clock time or mean solar time on successive days of a year. Using the same apparent solar time does not produce the same east–west equation-of-time offset. The international name Betelgeuse is preferable for a concise star label.
α: right ascension (0–24h, eastward from the vernal equinox)
δ: declination (-90°~+90°)
ε = 23.44° (obliquity)
Celestial and geographic coordinates compared: Right ascension ≈ longitude, declination ≈ latitude Reference plane: celestial equator (extension of Earth's equatorial plane)
Concept explanation
—
Current celestial object position
Right ascension α—
Declination δ—
Ecliptic longitude λ (approx.)—
Ecliptic latitude β (approx.)—
Reference objects
Betelgeuseα5h55m δ+7.4°
Siriusα6h45m δ-16.7°
Vegaα18h37m δ+38.8°
Polarisα2h32m δ+89.3°
Antaresα16h30m δ-26.4°
Vernal equinox γα0h δ0°
Counterintuitive insight
The celestial equator and Earth's equatorare not in the same plane— the celestial equator is the great circle formed by projecting Earth's equator onto the celestial sphere, but the celestial equator and the ecliptic intersect at the vernal and autumnal equinoxes, at an angle equal to the obliquity of 23.44°.
Polaris has declination ≈ +89.3°, not exactly +90° — the true north celestial pole shifts due to precession, completing a cycle in about 26000 years.