Unit 1 - Lesson 3: Orientations in the Night Sky
Type:
E-book, Lesson PlanDescription:
This lesson is part of the Athabasca University Astronomy 230: Northern Lights, Northern Skies course. In this lesson, you will learn how to describe the advantages of the altitude-azimuth system of reference and the equatorial coordinate system of reference, and how to describe how to determine the location of a star in the sky using both the altitude-azimuth system and the equatorial coordinate system.
Subjects:
- Science > General
- Science > Astronomy
Education Levels:
- Grade 11
- Grade 12
- Higher Education
- Graduate
- Undergraduate-Upper Division
- Undergraduate-Lower Division
Keywords:
astronomy earth pole axis orbit solstice equinox altitude azimuth zenith declination ascension constellation celestial sphere Polaris circumpolar motionLanguage:
EnglishAccess Privileges:
MembersLicense Deed:
Creative Commons Attribution 3.0Objectives
To an untrained observer, the night sky is full of small points of light. Some make recognizable patterns, which can be described so that others can find them. But how do you describe exactly where a particular star is found in the sky? There are two systems of reference used by astronomers to locate any object in the sky.
The altitude-azimuth system is based on the observer, and what he or she can see from his or her location. Imagine standing in the middle of a field, facing due north, and imagine a bright star just off to the right. The location of that star can be described using two coordinates: in what horizontal (or cardinal) direction it is found (azimuth), and how high up in the sky it is (altitude). Both coordinates are measured in degrees.
The altitude is measured from the horizon upward to the object, and goes no higher than 90? – anything at a greater angle starts coming back down toward the horizon. Right on the horizon, a star would have an altitude of 0?. An altitude of exactly 90? brings you to the point directly above your head, and is called the zenith. If your star is about halfway between the horizon and the zenith, above your head, its altitude would be 45?.
The azimuth is measured from the point on the horizon due north and moving eastward to the point directly under your star and goes to a maximum of 360?– an azimuth of 360? brings you back to due north.
In order to find a star with an azimuth of 64 degrees and an altitude of 31 degrees, you would begin by facing due north. Turn to the right (eastward) 64 degrees, and then look about a third of the way from the horizon to the zenith.
While this is a straightforward system of reference, it is not very practical. While you might observe a star at an azimuth of 64 degrees and an altitude of 31 degrees, an observer at any other location on the Earth would have to use slightly different coordinates based on their position. Further, since the stars appear to revolve around the Earth, even from your location, your bright star will find itself at different coordinates within the hour.
What is required is a coordinate system that does not depend on the observer, but on a fixed reference point that does not change over time. For points on the Earth, longitude and latitude coordinates serve this purpose – a city located at 113 degrees west and 55 degrees north will always be located at 113 degrees west and 55 degrees north, whether you are traveling to it from Vancouver, British Columbia, or Iqaluit, Nunavut. The equatorial coordinate system does the same for points in the sky.
Declination (or, dec) is used instead of latitude, and measures a star’s north-south position relative to the celestial equator. Recall that the equator is a fixed object, relative to the Earth. A positive declination indicates being north of the equator, while a negative declination indicates being south of the equator. Just like altitude, declination is measured in degrees, up to +/- 90 degrees. Polaris, being directly above the north celestial pole, would have a declination of +90 degrees.
Right Ascension (or, RA), is used instead of longitude. It measures the east-west position of a star relative to the point where the Sun crosses the equator on the vernal equinox. This is a point that remains fixed relative to the Earth, and is analogous to the point on the Earth where the Prime Meridian passes through the equator – all longitudinal readings are based on their distance east or west of that point. So, too, is the right ascension measured for stars. RA is measured in hours, minutes and seconds of the vernal equinox, moving eastward along the equator. 24 hours is equivalent to 360?.
While the equatorial coordinate system is not as simple as the altitude-azimuth system, its elegance lies in the fact that is fixes stars’ locations in the sky, regardless of the location of the observer, the time of day or the annual motions of the Earth around the Sun.
Did you know?
Although it was first used as far back as the 2nd century by the Greek scientist Hipparchos, the equatorial coordinate system was not widely used until the invention of the telescope in the early 1600s. Telescopes are often mounted on an “equatorial mount,” which allows the telescope to rotate across the sky in the same way the stars appear to move. As more astronomers began using telescopes with these mounts, the equatorial coordinate system was adopted for general use. Today, it is the most widely used coordinate system by both professional and amateur astronomers.
- describe the advantages of the altitude-azimuth system of reference and the equatorial coordinate system of reference
- describe how to determine the location of a star in the sky by using both the altitude-azimuth system and the equatorial coordinate system
To an untrained observer, the night sky is full of small points of light. Some make recognizable patterns, which can be described so that others can find them. But how do you describe exactly where a particular star is found in the sky? There are two systems of reference used by astronomers to locate any object in the sky.
Big and Little Dippers
The altitude-azimuth system is based on the observer, and what he or she can see from his or her location. Imagine standing in the middle of a field, facing due north, and imagine a bright star just off to the right. The location of that star can be described using two coordinates: in what horizontal (or cardinal) direction it is found (azimuth), and how high up in the sky it is (altitude). Both coordinates are measured in degrees.
The altitude is measured from the horizon upward to the object, and goes no higher than 90? – anything at a greater angle starts coming back down toward the horizon. Right on the horizon, a star would have an altitude of 0?. An altitude of exactly 90? brings you to the point directly above your head, and is called the zenith. If your star is about halfway between the horizon and the zenith, above your head, its altitude would be 45?.
The azimuth is measured from the point on the horizon due north and moving eastward to the point directly under your star and goes to a maximum of 360?– an azimuth of 360? brings you back to due north.
Locating a star using altitude and azimuth
In order to find a star with an azimuth of 64 degrees and an altitude of 31 degrees, you would begin by facing due north. Turn to the right (eastward) 64 degrees, and then look about a third of the way from the horizon to the zenith.
While this is a straightforward system of reference, it is not very practical. While you might observe a star at an azimuth of 64 degrees and an altitude of 31 degrees, an observer at any other location on the Earth would have to use slightly different coordinates based on their position. Further, since the stars appear to revolve around the Earth, even from your location, your bright star will find itself at different coordinates within the hour.
What is required is a coordinate system that does not depend on the observer, but on a fixed reference point that does not change over time. For points on the Earth, longitude and latitude coordinates serve this purpose – a city located at 113 degrees west and 55 degrees north will always be located at 113 degrees west and 55 degrees north, whether you are traveling to it from Vancouver, British Columbia, or Iqaluit, Nunavut. The equatorial coordinate system does the same for points in the sky.
Declination (or, dec) is used instead of latitude, and measures a star’s north-south position relative to the celestial equator. Recall that the equator is a fixed object, relative to the Earth. A positive declination indicates being north of the equator, while a negative declination indicates being south of the equator. Just like altitude, declination is measured in degrees, up to +/- 90 degrees. Polaris, being directly above the north celestial pole, would have a declination of +90 degrees.
Right Ascension (or, RA), is used instead of longitude. It measures the east-west position of a star relative to the point where the Sun crosses the equator on the vernal equinox. This is a point that remains fixed relative to the Earth, and is analogous to the point on the Earth where the Prime Meridian passes through the equator – all longitudinal readings are based on their distance east or west of that point. So, too, is the right ascension measured for stars. RA is measured in hours, minutes and seconds of the vernal equinox, moving eastward along the equator. 24 hours is equivalent to 360?.
Locating a star using right ascension and declination.
While the equatorial coordinate system is not as simple as the altitude-azimuth system, its elegance lies in the fact that is fixes stars’ locations in the sky, regardless of the location of the observer, the time of day or the annual motions of the Earth around the Sun.
Did you know?
Although it was first used as far back as the 2nd century by the Greek scientist Hipparchos, the equatorial coordinate system was not widely used until the invention of the telescope in the early 1600s. Telescopes are often mounted on an “equatorial mount,” which allows the telescope to rotate across the sky in the same way the stars appear to move. As more astronomers began using telescopes with these mounts, the equatorial coordinate system was adopted for general use. Today, it is the most widely used coordinate system by both professional and amateur astronomers.
