About 23.5 degrees.
The celestial equator and the ecliptic are two "great circles" on the sky coordinate system.
Think of them as two hoops of the same size, hinged together at two points (well the hinged points do move but very slowly taking about 26 000 years to move around and come back to the same place again). If you hold one
steady and spin the other one inside it, they stay connected at the two hinges, but they can
be set at any angle to each other.
Now put them in the sky. Place the steady one right above the equator all the way around, and tilt
the movable one on the hinges so that it makes an angle of 23.5 degrees with the steady one.
The steady one, above the earth's equator all the way around, is the celestial equator. The movable one,
tilted 23.5 degrees to the equator, is the ecliptic ... the path that the sun appears to travel in the sky,
once around in a year. The hinges ... where the ecliptic crosses the equator ... are the points where the
sun is located at the time of the two equinoxes. Halfway between the hinges are the points where the
two circles are farthest apart ... one where the ecliptic is farthest above the equator, the other where
it's farthest below. Those are the points where the sun is located at the time of the two solstices.
Inclination is measured as the angle at which the satellite crosses the equator while passing from the southern hemisphere to the northern hemisphere. Declination is the difference between magnetic North as reported by a compass and true North.
The plane of Earth's orbit is known as the ecliptic. It is the flat plane in space that represents the path along which the Earth travels around the Sun. The ecliptic is inclined at an angle of approximately 23.5 degrees to the celestial equator.
Latitude. It is the angular distance measured in degrees north or south of the equator.
The pole is at 90 degrees North. The summer solstice happens when the Sun is overhead at the maximum latitude it ever reaches North (the Tropic of Cancer) which is currently 23° 26′ 16″ north of the Equator. Therefore the angular distance of the Sun from the North celestial pole at the summer solstice is (90° - 23° 26′ 16″ )= 66° 33′ 44″ measured from the pole.
Distance (angular) from the poles (or the equator).
Those would be the "equinoxes".
The angle between the equinoctial and the ecliptic is known as the obliquity of the ecliptic. It is the angle between the plane of Earth's orbit around the Sun and the plane of the celestial equator. Currently, the obliquity of the ecliptic is about 23.5 degrees.
Inclination is measured as the angle at which the satellite crosses the equator while passing from the southern hemisphere to the northern hemisphere. Declination is the difference between magnetic North as reported by a compass and true North.
It's because the Earth's axis is tilted. Therefore the plane of the equator is tilted (at about 23.5 degrees) away from the plane of the Earth's orbit. Therefore the celestial equator is tilted away from the ecliptic.
It's because the Earth's axis is tilted. Therefore the plane of the equator is tilted (at about 23.5 degrees) away from the plane of the Earth's orbit. Therefore the celestial equator is tilted away from the ecliptic.
The celestial line that is a product of Earth's rotation is the celestial equator. It is an imaginary line located above Earth's equator and is created as a result of Earth's rotation on its axis. It divides the celestial sphere into northern and southern hemispheres.
Declination (positive and negative respectively) is the angular distance between north and south of the Celestial Equator.
celestial equator
the angular distance of a place north or south of the earth's equator, or of a celestial object north or south of the celestial equator, usually expressed in degrees and minutes
A declination is a term used in astronomy to describe the angular distance of a celestial object from the celestial equator. For example, the declination of the star Sirius is approximately -16.7 degrees, indicating its position relative to the celestial equator.
The places where the ecliptic crosses the equator are called the vernal equinox (where the Sun crosses from south to north) and the autumnal equinox (where the Sun crosses from north to south). These are the points where day and night are equal in length, marking the beginning of spring and autumn, respectively.
You measure the angles from east from the first point of Aries (which is the place in the sky where the Sun crosses the celestial equator at the March equinox) and north from the ecliptic (declination).