This Orbital Velocity calculator simply calculates eccentricity, orbital energy, radius, and speed of planets using semi-major axis, semi-minor axis, start mass, satellite mass, period, and distance information.

**Orbital Velocity Calculator:** The orbital velocity calculator is a sophisticated tool for calculating planet motion parameters in elliptical orbits or on circular orbit. Do you wish to know the Earth's orbital velocity or the time of Jupiter's orbit? Our orbital velocity calculator allows you to rapidly calculate: orbital radius, orbital energy, orbital speed, and orbital period of the planets are all measured in kilometres. Also, you need enter the star's (e.g., Sun's) and satellite's masses (e.g., Mars, Moon). The orbital velocity equation and the Kepler principles can be used to calculate it. Finally, the so-called vis-viva equation might be used.

It is related to the other two key parameters: semi-major axis and semi-minor axis with the eccentricity formula is **e = √(1 - b ^{2}/a^{2})**.

**V _{e} = [2GM/R]V **

- where, The eccentricity is denoted as e
- The semi-major axis is denoted as a
- The semi-minor axis is denoted as b
- We can calculate periapsis and apoapsis

**Periapsis:**The closest possible distance of the satellite (planet) to a star.

**Apoapsis:** The farthest possible distance of the satellite (planet) to a star using the given parameters.

With the following elliptical orbit definition, we may estimate distances to a star at periapsis and apoapsis:

**ra+rp = 2*a**

**ra*rp = b ^{2}**

- where, ra is the distance between the star and the satellite in apoapsis
- rp is the distance between the star and the satellite in periapsis

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The speed at which one body spins around another is known as orbital velocity. Objects in orbit are those that travel in a consistent circular motion around the Earth. The distance between the object and the earth's centre determines the orbit's velocity.

This velocity is frequently assigned to artificial satellites in order for them to rotate around a specific planet.

The formula for orbital velocity is as follows: **V _{orbit} = √GM/R**

Where,

- G stands for gravitational constant
- M is the mass of the body at its centre
- R is the orbit's radius

If mass M and radius R are known, the Orbital Velocity Formula is used to compute the orbital velocity of any planet.

The unit of the orbital velocity is measured in metre per second (m/s).

We can model the motion of orbiting satellites using the vis-viva equation. It calculates a satellite orbital speed at any point on an elliptic orbit, as well as its orbital velocity in periapsis and apoapsis.The following is the vis-viva equation:

**V ^{2} = μ*(2/r-1/a)**

- Here, v be the relative satellite speed
- μ be the standard gravitational parameter μ = G(M + m)
- The gravitational constant and it is denoted by G and the value is 6.674 x 10
^{-11 }N-m^{2}/kg^{2}. - M is the mass of the star
- The mass of the satellite denoted as m
- r is the distance between the star and the satellite
- a is the semi-major axis of the elliptical orbit

You may calculate the satellite speed at apoapsis (r = ra) and periapsis (r = rp) using the orbital speed formula above.

You calculate orbital period of planets that can be derived from the Kepler laws of planetary motion:

The law of orbits is Kepler's first law: Every planet in the Solar System follows an elliptical orbit around the Sun.

The law of areas is Kepler's second law: A line segment between a planet and the Sun sweeps out equal portions at equal intervals (area speed is constant).

The law of periods is Kepler's third law. By comparing the centripetal force to the gravitational force, you may get the simplified form of Kepler's third law. The complete equivalent formula is as follows:

**T ^{2}=4*π^{2}*a^{3}/μ**

- Here, T be the orbital period of a satellite
- To determine the orbital energy of planets by the following formula is E=-G*M*m/(2*a).
- Planets have a negative total orbital energy that is independent of the ellipse's eccentricity.

**Question 1:** Find the orbital eccentricity whose semi-major and semi-minor axis are 100m and 50m.

**Solution:**

Consider the problem, we have

Semi-major axis, a = 100m

Semi-minor axis, b = 50m

The formula for finding the Eccentricity, **e = √(1 – b ^{2}/a^{2})**

e = 0.8660254037844386

e = 0.87

Therefore,the orbital eccentricity is **0.8660254037844386**

**1. What does orbital velocity imply?**

The speed necessary to achieve orbit around a celestial body, such as a planet or a star, is known as orbital velocity. This necessitates travelling at a constant speed that: Aligns with the rotational velocity of the celestial object.

**2. Is orbital velocity and orbital speed the same factor?**

The distance between the item and the Earth's centre determines the orbit's velocity. The velocity must be just correct such that the distance to the Earth's centre remains constant. As a result, orbital speed is a crucial calculation.

**3. What is the earth and satellite orbital velocity?**

The Earth's orbital velocity is 29.78 kilometres per second. A satellite's orbital velocity is 17,000 metres per hour.

**4. Define orbital velocity and Its formula.**

The speed at which one body spins around another is known as orbital velocity. Objects in orbit are those that travel in a consistent circular motion around the Earth. The distance between the object and the earth's centre determines the orbit's velocity.

The formula for orbital velocity is as follows:**V _{orbit} = √GM / R.**

**5. What is the required velocity to remain in orbit?**

A satellite must travel at an extremely high velocity, which varies depending on its height, to stay in orbit. A speed of 7.8 km/s (28,000 km/h) is required for a circular orbit at a height of 300 km above the Earth's surface. The spacecraft will complete one orbit around the Earth in 90 minutes at current speed.