Physics planetary motion how to review, planetary motion physics questions

In order to get good grades, many students participate in various tutoring and review very carefully, but their academic performance just can't be improved. Because they used the wrong method for revision, their brains were not very good. Here are some ideas for you on review:

1. Chapter review, no matter which discipline is divided into large chapters and small class hours, generally when all the lessons of a chapter are finished, the entire chapter will be strung together in the system to talk about it again, as a review, we can also do this, because since it is a chapter of knowledge, all the lessons must be connected before, so we can find out what they have in common, and use the contact memory method to string these fragmented knowledge through the line, which is more convenient for us to remember.

2. Error correction: It is inevitable to make mistakes in the process of the exam, whether you are careless or just not, you must habitually collect these wrong questions, and each subject establishes an independent set of wrong questions, when we review before the exam, they are the key review objects, so since you miss once, you may not be wrong the second time, only in this way will you not lose points again on the same issue.

3. If you want to improve your academic performance faster, you can improve your memory and comprehension. I used to have a very poor memory, my grades were not satisfactory, and I often failed exams. It wasn't until I ** "Nikolai Potential Training" that my fate changed.

After the training of the course, my memory, comprehension, and imagination have all improved. I mastered the skills of using my brain efficiently, and since then, I have stopped attending tutoring classes, and basically all my knowledge has been acquired through self-study. I easily studied various subjects on my own, and my academic performance improved by leaps and bounds, and I was finally admitted to university.

I hope my words can help you, hope!

Yes, but the period is measured in a circle around the Earth.

Let the planetary mass be m

The radius r is obtained by the gravitational excitation cavity of the pure cons of the Gongming pants style.

gm/r^2=4r∏^2/t^2

t^2=4∏^2

r^3/gm

m=pv=p(4∏r^3/3)

t^=3∏/gp

pt^2=3∏/g=k

Not bad, I hope you do.

One more week and two more weeks are all encounters, the difference is: one more week is the first encounter thereafter, two more weeks is the second time, and so on;

The problem is that you misunderstood, one more week does not mean that A turns two times and B only turns once, but after (the still unknown time between the pants, the unknown circle), A finally turns this one more circle than B (so it gets closer again), like the champion in the 50,000-meter race may throw off the lagging runner by one lap or even two or three laps (at that time it was the first of the two runners.

two or three encounters);

In the same way, when two stars are furthest apart, their number of revolutions is half a turn;

The angular velocity of the reed wheel of planet a is 1=2 t1

The angular velocity of planet b is 2=2 t2

Then A is behind B or B is one week behind A, which is 2

t1=2π/|1-ω2|=t1t2/|t1-t2|Calculate the farthest distance of the first accompaniment letter, and the lead banquet will be half a week

t2=π/1-ω2|=t1t2/（2|t1-t2|）

It is impossible to find out, the period is only related to the mass of the celestial body being orbited, and the radius of the motion of the celestial body.

One more week, more than two weeks, three weeks are all encounters, the difference is: one more week is the first encounter thereafter, two more weeks is the second, and so on;

The problem is that you misunderstood, an extra week does not mean that A turns two times and B only makes one turn, but after (now unknown time, unknown laps), A finally turns this way more than B (so it gets closer again), like in the 50,000-meter race, the champion may throw off the lagging runner by one or even two or three laps (at that time, it was the first of the two runners).

two or three encounters);

In the same way, when two stars are furthest apart, their number of revolutions is half a turn;

Let the planetary mass be m and the radius be r

Obtained from the formula of gravitational force.

gm/r^2=4r∏^2/t^2

t^2=4∏^2 r^3/gm

m=pv=p(4∏r^3/3)

t^=3∏/gp

pt^2=3∏/g=k

Not bad, I hope you adopt it.

The angular velocity of planet a is 1=2 t1

The angular velocity of planet b is 2=2 t2

Then A is behind B or B is one week behind A, which is 2

t1=2π/|ω1-ω2|=t1t2/|t1-t2|The calculation of the farthest distance for the first time will be half a week

t2=π/|ω1-ω2|=t1t2/（2|t1-t2|）

You read it wrong.

Be an extra week to go.

Not a week of walking.

If there is no encounter.

Can you walk for an extra week.

If you meet.

Isn't that an extra week away.

(2 t1-2 t2)t=2 t=(t2-t1) t1t2

Because it was the first encounter, it was a week, and the farthest distance was just one diameter, that is, half a week.

Planetary motion. Why the Sun, Moon and planets move on the celestial sphere. We can imagine the sky as a large glass sphere called the celestial sphere, on which all celestial bodies, including the sun and stars, are inlaid and the earth is alone.

When the earth rotates from west to east, humans on the earth do not feel the movement of the earth, but feel that the entire celestial sphere revolves around the earth from east to west, creating the illusion that the sun and other celestial bodies rise in the east and set in the west every day.

Stars close to the celestial north pole never go down, and we call these stars arch poles. Polaris is just one of many arch pole stars, and since it is so close to the celestial North Pole, it seems to be forever stationary.

The position of the North Star relative to the ground depends on the latitude of the observer's location. People in the Northern Hemisphere do not see stars close to the southern celestial pole, and people in the Southern Hemisphere do not see stars close to the northern celestial pole.

Due to the Earth's orbital motion, the position of the Sun on the celestial sphere moves from west to east all the time, and it orbits the celestial sphere once a year. The trajectory of the Sun on the celestial sphere is called the ecliptic, and the constellations on the zodiac are called the zodiac, which derives from ancient astrology.

What is a day?

It is generally assumed that the sun returns to the same position relative to the ground as a day, for example, from noon to another noon, and the day defined in this way is called a solar day. A sundial, which measures time by projecting the position of the sun, is a timekeeping instrument that operates according to this definition. Another definition is a day when the stars return to the same position in the sky, which is called a sidereal day.

Due to the rotation of the Earth, a solar day is longer than a sidereal day, and there are about 365 solar days in a year, but there are 366 sidereal days.

To be precise, there are solar days in a year, and in order to avoid errors caused by the long-term accumulation of this day, the solution of a four-year leap year is used, and the ordinary year is 365 days, and the leap year has 366 days, and the extra day is placed on the last day of February. A 4-year leap year has an average of days, which is more than the true number of days in a year, and the error accumulated over hundreds of years is not small, so the calendar stipulates that years that can be divided by 100 are not intercalated (e.g., ), and years that can be divided by 400 are kept intercalary (e.g., ). Thus, every 400 years there are 3 leap years missing, that is, the average year is less than a day, and the error is a day per year, and the error is almost one day every 3000 years.

This calendar is called the Gregorian or Grigan calendar.

The apparent motion of the Moon. The difference between two full moons is called a wax and fall month. The lunar calendar used by the Chinese already takes into account the movement of the sun and the moon, so it is correctly said to be a lunisolar calendar.

Because the Earth's axis of rotation is tilted relative to the plane of its orbit, coupled with the Earth's motion around the Sun, the azimuth angle of the Sun's eastward rise changes with the day.

Deal with Kepler's third law.

The spacecraft returns to the ground in an elliptical orbit, and the symmetry suggests that the time required for the spacecraft to move from A to B should be half of its cycle.

Let the period of the spacecraft's motion along an elliptical orbit be t

Half-length noisy car axle = (r+r) 2

t r =t' [r+r) 2] solution: t =t (r+r) 8r write it yourself.

The time it takes for point A to return to point B is t' 2