Horizontal system of celestial coordinates

In summary, the conversation discusses how the horizontal system of celestial coordinates can be used to find the location of the north celestial pole from an observer's perspective based on their latitude. It also mentions that the south celestial pole is not visible from locations north of the equator.
  • #1
suedenation
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given the latitude and longitude of a place, how can you use the horizontal system of celestial coordinates to find the location of the north celestial pole from an observer standing on that place?

For me, it's quite hard to imagine the Earth as a sphere, if 2-dimension, it's fine for me. How about you guys?
 
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  • #2
It's their latitude. For example, at the North Pole, latitude 90, the North celestial pole is 90 degrees from the horizon. From San Francisco, latitude 38 degrees, the north celestial pole is 38 degrees above the northern horizon. The south celestial pole is not visible from here, or anywhere north of the equator.
 
  • #3


The horizontal system of celestial coordinates is a way of locating objects in the night sky relative to an observer's position on Earth. It uses two coordinates, altitude and azimuth, to pinpoint the location of celestial objects. Altitude is the angle above the horizon and azimuth is the angle measured clockwise from north.

To find the location of the north celestial pole from an observer's position, we first need to determine the observer's latitude and longitude. This can be done using a map or a GPS device.

Once we have the latitude and longitude, we can use the altitude and azimuth coordinates to locate the north celestial pole. The altitude of the north celestial pole will always be equal to the observer's latitude. For example, if the observer's latitude is 40 degrees north, then the altitude of the north celestial pole will also be 40 degrees above the horizon.

To find the azimuth of the north celestial pole, we need to use the following formula: azimuth = 180 degrees - (longitude + 90 degrees). For example, if the observer's longitude is 80 degrees west, then the azimuth of the north celestial pole would be 180 degrees - (80 degrees + 90 degrees) = 10 degrees.

Using these coordinates, an observer can easily locate the north celestial pole in the night sky. This is an important reference point for stargazing and can also be used to determine the direction of true north.
 

What is a horizontal system of celestial coordinates?

A horizontal system of celestial coordinates is a way of describing the positions of celestial objects (such as stars, planets, and galaxies) relative to the observer on Earth. It uses the observer's horizon as the reference point and measures the altitude (angle above the horizon) and azimuth (angle along the horizon) of an object.

How does the horizontal system differ from other coordinate systems?

The horizontal system differs from other coordinate systems, such as equatorial and ecliptic coordinates, in that it is observer-centered. This means that the coordinates of an object will appear different to different observers on Earth, depending on their location and time of observation.

What are the advantages of using the horizontal system?

One advantage of the horizontal system is that it is more intuitive for observers on Earth, as it uses the horizon as a reference point. It also allows for easy identification and tracking of objects as they rise and set in the sky, making it useful for navigation and amateur astronomy.

What is the relationship between the horizontal system and the celestial sphere?

The celestial sphere is a model used to represent the apparent positions of celestial objects as seen from Earth. The horizontal system is a way of projecting the celestial sphere onto the observer's local horizon, allowing for easy visualization and measurement of celestial objects.

Are there any limitations to the horizontal system?

One limitation of the horizontal system is that it is only useful for describing the positions of objects as seen from a specific location and time on Earth. This means that it cannot be used for precise astronomical measurements or for objects that are in motion relative to Earth, such as satellites.

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