# How to calculate mass of the sun? Please tell in a simple methamatical way.

You can calculate the mass of the Sun from Newton's form of Kepler's 3rd law.

The orbit of a planet around the Sun is described by Newton's version of Kepler's third law, which uses the following equation to connect the orbit's semi major axis distance to its period:

Thus, it implies:

Where a is the orbit semi major axis distance, M is the Sun's mass, p is the orbital period, and G is the gravitational constant.

After rearranging the equation, we get:

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The mass of the Sun can be calculated using the gravitational force equation:

[ F = \frac{{G \cdot m_1 \cdot m_2}}{{r^2}} ]

Where:

- ( F ) is the gravitational force between two objects,
- ( G ) is the gravitational constant ((6.674 \times 10^{-11}) m³/kg/s²),
- ( m_1 ) and ( m_2 ) are the masses of the two objects (in this case, the mass of the Sun and the mass of another object, for example, a planet),
- ( r ) is the distance between the centers of the two objects.

Rearranging the equation to solve for the mass of the Sun (( m_1 )):

[ m_1 = \frac{{F \cdot r^2}}{{G \cdot m_2}} ]

By measuring the gravitational force (( F )) experienced by an object (such as a planet) orbiting the Sun at a known distance (( r )), and knowing the mass of the object (( m_2 )), we

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When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.

When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.

When evaluating a one-sided limit, you need to be careful when a quantity is approaching zero since its sign is different depending on which way it is approaching zero from. Let us look at some examples.

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