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17 Exakte Antworten 4 Text Antworten 21 Multiple Choice Antworten
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The declination of the sun is defined as

The angular distance of the sun north or south of the celestial equator.

The arc from the celestial horizon to the sun measured along a vertical line perpendicular on the horizon.

The arc of the meridian of the sun measured from the nearest pole to the sun.

The arc along the celestial sphere from zenith to the sun.

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By the term "transit" of a heavenly body it is understood that:

the body is passing the meridian of the observer or another specified meridian

the body is passing the anti meridian of the observer

the body is moving

the body is at the same celestial meridian as another body

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Which is the highest latitude listed below at which the sun will rise above the horizon and set every day?

66,5 Grad
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Observed from a position on the surface of the Earth the heavenly bodies seems to

move from east to west

move from east to west on the northern hemisphere

move from west to east on the southern hemisphere

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Above what latitude is the sun in zenith at the spring equinox on the northern hemisphere?

The Equator

N 66° 33'

N 23° 27'

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The term "Sidereal Hour Angle" (SHA) is used

to define the position of a star on the celestial sphere without reference to Earth co-ordinates

to describe the time interval between two successive transits of the real apparent sun at the same meridian

to describe the position of a star with reference to the moon

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Assuming mid-latitudes (40° to 50°N/S). At which time of year is the relationship between the length of day and night, as well as the rate of change of declination of the sun, changing at the greatest rate?

Spring equinox and autumn equinox

Summer solstice and spring equinox

Winter solstice and autumn equinox

Summer solstice and winter solstice

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The sun's declination is

The sun's position relative to the plane of the Equator

The angular distance between the sun and the celestial North Pole

The distance between the sun and the horizon

The sun's position relative to the ecliptic

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What is meant by "Aphelion"?

The point of the earth's orbit furthest away from the sun.

The point of the sun's orbit closest to the earth.

The point of the earth's orbit closest to the sun

The point of the sun's orbit furthest away from the earth.

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If the LMT in position 54°40’S 000°00’ is 15:25, what is the GMT in position 54°40’S 180°00’?

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The greatest difference between the length of the apparent solar day and the mean solar day occur

February and November

January and July

October and May

March and September

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A day is defined as

the period elapsed between two successive transits of a heavenly body

the period from sunrise to sunset

the period from morning to evening

the period in which day flying is authorised

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The mean sun

Moves with constant speed along the celestial equator

Has a declination equal to the apparent sun

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"Mean time" has been introduced in order to

Introduce a constant measurement of time, independent of the daily variations in the movement of the Sun as observed from the Earth

Compensate for the irregularities of the speed of rotation of the Earth around it's axis

Save us the problem of adjusting our watches entering every leap year

Have one fixed time to be used within the border of a country

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The International Date Line is located

At the 180°E/W meridian, or in the vicinity of this meridian

At all latitudes on the 180°E/W meridian

At the Greenwich meridian

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The length of a apparent solar day is not constant because:

the Earth's speed of revolution in its orbit varies continuously, due to the orbit being elliptical

the plane of the Ecliptic and the plane of the Equator are inclined to each other

the Earth's speed of rotation is not the same at all latitudes

the Sun's declination is not constant

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The "Equation of time"

states the difference in time of transit of the Mean sun and the Apparent sun any particular day

is used when calculating the difference between UTC and LMT

states the difference between celestial time and apparent time

is used to calculate mean time when standard time is known

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The Analemma 

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North south difference is due to the tilt of the earth rotational axis on its orbit around the sun ==> the east west difference is due to the ecliptic
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mean solar day

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the time between two successive transit of the mean sun on the meridian of the specified location
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The reak sun lags behind around which day?

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max. 12 February and 27 july
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The real sun leads around which day?

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max. 4 november and 15 may
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137 Grad 36 Min    In hour ANgle?

137,36 in den Taschenrechner ==> DMS DD ==> Resultat / 15 ==> dd zu DMS 360 Grad = 24h 15 Grad = 1h
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the earth closest to the su around January 4 at about 147 Mio km ==> Im Winter
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The Earth furthest away from the sound ==> am 5 July => Sommer
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Keplers Law 1 und 2?

1. The Law of Orbits;

2. the law of areas:

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Kepler: 1. The Law of Orbits;


all planets move in elliptical orbits, with the sound at one focus ==> F = G x ((m1 x m2)/distance^2) G = universal gravitation constant
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Kepler:  2. the law of areas:

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A line that connects a planet to the sun sweeps out equal areas in equal times ==> Geschwindigkeit um die SOnne unterschiedlich zwischen Winter und Sommer ==> Geschwindigkeit nimmt zu, weil r klein wird und mc und 1 gleich gross sein müssen
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senkrecht über uns => bzw wenn die Sonne über uns ist ==> Reffs to an imaginary point directly above a particular location on geh imaginary celestial sphere
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declinatiion is ?

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teh angular distance of a heavenly body above N or below S the celestial equator
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Sidereal year anzahl Tage?

interval of time for the Earth to orbit the Sun once with respect to the fixed start ==> 365d 06h 09 s 09 ms