Calculate gravitational and relativistic time dilation for two observers.
Observer 1
The mass of the object (e.g., planet or star) affecting Observer 1, in kilograms.
This determines the strength of the gravitational field. For example, Earth's mass is approximately 5.972 × 10²⁴ kg.
Larger masses cause greater gravitational time dilation, slowing time for the observer.
The distance from the center of the massive object to Observer 1, in meters.
This is typically the radius of the planet or star. For example, Earth's radius is about 6.371 × 10⁶ m.
Smaller radii (closer to the mass) increase gravitational time dilation.
The speed of Observer 1 relative to a stationary reference frame, in meters per second.
This affects relativistic time dilation. For example, a velocity of 0 m/s means no relativistic effects,
while high speeds (e.g., 0.5 × speed of light) significantly slow time. Must be less than 299,792,458 m/s.
Observer 2
The mass of the object affecting Observer 2, in kilograms.
For example, a planet 100 times Earth's mass would be 5.972 × 10²⁶ kg.
This influences gravitational time dilation, with larger masses causing greater time dilation.
The distance from the center of the massive object to Observer 2, in meters.
For example, using Earth's radius (6.371 × 10⁶ m) assumes Observer 2 is on the surface.
Smaller distances amplify gravitational time dilation effects.
The speed of Observer 2 relative to a stationary reference frame, in meters per second.
High velocities cause relativistic time dilation, slowing time for the observer.
Set to 0 for no relativistic effects. Must be less than the speed of light (299,792,458 m/s).
The time experienced by a reference observer in a weak gravitational field and at rest, in seconds.
For example, 86,400 seconds equals 1 day. This is the baseline time used to calculate how much
time each observer experiences after dilation effects are applied.