Handleiding Celestron CPC Deluxe 1100 HD - 11009 (pagina 37 van 50) (Engels)

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Celestial pole The imaginary projection of Earth’s rotational axis

north or south pole onto the

celestial sphere.

Celestial An imaginary sphere surrounding the Earth,

Sphere concentric with the Earth’s center.

Collimation The act of putting a telescope’s optics into perfect

alignment.

D –

Declination The angular distance of a celestial body

(DEC) north or south of the celestial equator. It may

be said to correspond to latitude on the

surface of the Earth.

E –

Ecliptic The projection of the Earth’s orbit on to the celestial

sphere. It may also be dened as “the apparent

yearly path of the Sun against the stars.”

Equatorial A telescope mounting in which the instrument

mount is set upon an axis which is parallel to the

axis of the Earth; the angle of the axis must be

equal to the observer’s latitude.

F –

Focal length The distance between a lens (or mirror) and the point

at which the image of an object at innity is brought

to focus. The focal length divided by the aperture of

the mirror or lens is termed the focal ratio.

G –

GoTo Term used to refer to a computerized telescope

or to the act of slewing (moving) a computerized

telescope.

J –

Jovian Planets Any of the four gas giant planets that are at a greater

distance form the Sun than the terrestrial planets.

K –

Kuiper Belt A region beyond the orbit of Neptune extending

to about 1000 AU which is a source of many short

period comets.

L –

Light–Year (ly) A light–year is the distance light traverses in a

vacuum in one year at the speed of 186,000 mi/sec.

(299,792 km/sec.) With 31,557,600 seconds in a year,

the light–year equals a distance of 5.88 trillion miles

(9.46 trillion km).

M –

Magnitude Magnitude is a measure of the brightness of a

celestial body. The brightest stars are assigned

magnitude 1 and those increasingly fainter from

2 down to magnitude 5. The faintest star that can

be seen without a telescope is about magnitude 6.

Each magnitude step corresponds to a ratio of 2.5 in

brightness. Thus a star of magnitude 1 is 2.5 times

brighter than a star of magnitude 2, and 100 times

brighter than a magnitude 5 star. The brightest star,

Sirius, has an apparent magnitude of –1.6, the full

moon is –12.7, and the Sun’s brightness, expressed

on a magnitude scale, is –26.78. The zero point of the

apparent magnitude scale is arbitrary.

Meridian A reference line in the sky that starts at the North

celestial pole and ends at the South celestial pole and

passes through the zenith. If you are facing South,

the meridian starts from your Southern horizon and

passes directly overhead to the North celestial pole.

Messier A French astronomer in the late 1700s who was

primarily looking for comets. Comets are hazy

diuse objects and so Messier cataloged objects

that were not comets to help his search. This catalog

became the Messier Catalog, M1 through M110.

N –

Nebula Interstellar cloud of gas and dust. Also

refers to any celestial object that has a

cloudy appearance.

North Celestial The point in the Northern hemisphere around

Pole which all the stars appear to rotate. This is

caused by the fact that the Earth is rotating on

an axis that passes through the North and

South celestial poles. The star Polaris lies less

than a degree from this point and is therefore

referred to as the “Pole Star”.

Nova Although Latin for “new” it denotes a star that

suddenly becomes explosively bright at the end of its

life cycle.

O –

Open Cluster One of the groupings of stars that are concentrated

along the plane of the Milky Way. Most have

an asymmetrical appearance and are loosely

assembled. They contain from a dozen to many

hundreds of stars.

P –

Parallax Parallax is the dierence in the apparent position

of an object against a background when viewed

by an observer from two dierent locations. These

positions and the actual position of the object form

a triangle from which the apex angle (the parallax)

and the distance of the object can be determined

if the length of the baseline between the observing

positions is known and the angular direction of the

object from each position at the ends of the baseline

has been measured. The traditional method in

astronomy of determining the distance to a celestial

object is to measure its parallax.

Parfocal Refers to a group of eyepieces that all require the

same distance from the focal plane of the telescope

to be in focus. This means when you focus one

parfocal eyepiece all the other parfocal eyepieces, in

a particular line of eyepieces, will be in focus.

Parsec The distance at which a star would show parallax

of one second of arc. It is equal to 3.26 light–years,

206,265 astronomical units, or 30,800,000,000,000

km. (Apart from the Sun, no star lies within one

parsec of us.)

Point Source An object which cannot be resolved into an image

because it to too far away or too small is considered

a point source. A planet is far away but it can be

resolved as a disk. Most stars cannot be resolved as

disks, they are too far away.

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