What is the measurement of planetary distances??

The details are as follows: trigonometry is generally used, for example, the earth observes the angle of a star to the earth at the spring equinox and the autumn equinox, and then uses the orbital radius as the baseline to calculate its distance from the earth.

2.By measuring the closer stars, we can take the diameter of the Earth's orbit around the Sun as a baseline for a known distance.

The time it takes for the Earth to orbit the Sun is one year, and half a circle in half a year. In the two days when the first mill was half a year apart, the Earth was exactly at opposite ends of the diameter of the Earth's orbit. When the same star is observed in two days half a year apart, its direction is different, which is its parallax angle.

The distance of the star can be calculated from the parallax angle and the diameter of the Earth's orbit (300 million kilometers). With this method, only the distance of stars within two to three hundred light-years can be measured.

3.Stars farther away, because their parallax angles are too small to be measured, have to look for other methods. One of the famous methods is to use the circumferential relationship of Cepheids to calculate the distances of distant celestial bodies, which has earned Cepheids the nickname "Measuring Ruler".

Generally, trigonometry is used, for example, the Earth observes the angle of a Hengdian returning star to the Earth at the vernal and autumnal equinoxes, and then calculates its distance from the Earth with the radius of its orbit as the baseline.

4.Spectral redshift ranging method: The popular explanation for spectral redshift is the great cosmological theory.

Hubble pointed out that the redshift of celestial bodies is related to distance: z = h*d c, which is the famous Hubble's law, where z is the redshift; c is the speed of light; d is the distance; h is the Hubble constant, and its value is 50 80 kilometers (seconds·megaseconds).

According to this law, the distance d of the galaxy can be calculated as long as the redshift z of the extragalactic lineage is measured. Distances up to 10 billion light-years can be determined using the redshift method.

We've all heard that when talking about sidereal distances, the numbers involved are incredibly large. That is, how do we know how far away a star really is? While there are many ways to calculate the distance between our planet and another star, there are three that are the most effective.

Through simple mathematical and logical reasoning, our astronomers give us a more vivid picture of the universe. Now sit back, grab a cup of tea, and get your brain ready for some incredible math.

Have you ever noticed that when you look out the window at a moving car, objects close to you fly by, while objects far away from you seem to move slowly in comparison? This is called the parallax effect. In the same way, as we revolve around the Sun, the positions of stars closer to Earth move steadily from one position to another, while stars farther from Earth seem to move less frequently.

Using this principle, astronomers can calculate the distance to nearby stars with considerable accuracy. First, astronomers record the star's position in the night sky. Six months later, the position of the same star was measured again.

First, you have to understand an effect called parallax. If you hold up a finger in front of your nose, about 20 centimeters away from your nose, and then alternately open and close one of your eyes, this finger will look like jumping from side to side. This is because each eye gives you a different visual effect, and there is a few centimeters between your two eyes.

If you know two extremely important dimensions: the distance between your eyes and the angle at which your fingers appear to be jumping, then trigonometry will help you figure out how far your fingers are from your eyes. The problem is that this method is suitable for observing close fingers, but not for objects farther away.

If you try to do this to a lamppost at the end of a distant road, you will find that you can't detect any movement at all – it's too small to observe.

So, to increase parallax, the eyes must be more apart. Astronomers use this effect to make one observation at a point in the Earth's orbit and then make a second observation before the Earth reaches half a circle around its orbit (which takes about six months). Knowing the distance between these two observations gives you the distance from the Earth to the Sun, and the same method can measure the distance between a star and the Earth hundreds of light-years away.

Using the parallax effect, the distance between two points is measured.

Measurements are made through specific scientific methods and methods.

The first thing is to find two extremely demanding observation points, and secondly, to know the distance between the observation points, so that the distance between the stars can be calculated.

One observation is measured first, and then another, using the parallax effect.

Knowing the distance between these two observation points makes it possible to calculate the distance between stars hundreds of light-years away.

So, to increase parallax, the eyes must be more apart.

In the universe, all distance measurements are understood by the speed of light.

You have to understand an effect called parallax.

It is calculated by the interaction forces between the planets.

We can measure it with "trigonometric parallax". We can observe the same star at the spring and autumn equinoxes of the year, and we will find that the position of the star has changed. At this time, the star we can observe is the apex, connecting the position of the Earth at the time of the two observations, forming an angle, which is the annual parallax angle of the star.

The distance from the Earth to the Sun is called an astronomical unit. Divide one astronomical unit (100 million kilometers) by the annual parallax angle, which is the distance between the Earth and the star.

However, this method can only measure objects within 200,300 light-years. Stars farther away are undetectable because the parallax angle is too small. Therefore, to measure objects beyond 300 light years, you need to measure them according to standard candlelight or Cepheid variables, which I will introduce later.