PiMath.de Planetary Systems of the Earth 1
Classisc Systems
 
     
  Copyright © Klaus Piontzik  
     
 German Version    
German Version    

8.3.1 - The moons of Mars

In order to be able to clearly create an e-function, 3 data points are required. But Mars only has 2 moons. Since both moons orbit Mars relatively close, the surface of Mars can be used as a third value. The entire situation is given in the following table.

 

Name Radius Nr ln(Radius) Nr
        calculated
         

Mars equator

3396

0

8,13035355

0

Phobos

9376

1

9,14590851

1,05

Deimos

23459

2

10,0630095

2

 

When logarithmized and transferred to a diagram, a surprising simplification results. The logarithmic values ??are already so linear that further linearization is no longer necessary.

 

Linearization

Abbildung 8.3.6 – Linearization

 

As before, the e-function can be determined from this. The equation for the approximation line is:

y = ln R = 0.9963x + 10,407

The following applies to the orbits of the moon: R = 33096
e0.9663x [Km]

 

Moons of Mars

Illustration 8.3.7 – Moons of Mars

<

 to privuos page back home next  next page

 

 Planetary Systems 1

buy on Amazon

200 sides, 23 of them in color
154 pictures
38 tables

Production und Publishing:
Books on Demand GmbH, Norderstedt

ISBN 978-3-7357-3854-7

Price: 25 Euro

   

 

Der Autor - Klaus Piontzik