printf("Orbital Radius of Moon: %f E8 m \n", r_m/1E8);
printf("Orbital Radius of Moon: %f Moon Distances \n",
r_m/3.84E8);
printf("Radius of Moon: %f E6 m \n", R_m/1E6);
printf("Radius of Moon: %f Moon Radii \n", R_m/1.7374E6);
printf("Mass of Moon: %f E22 kg \n", M_m/1E22);
printf("Mass of Moon %f Moon Masses \n", M_m/
7.347673E22);
printf("density of moon: %f g/cm3 \n", MoonDensity);
printf("\n");
printf("\n");
v_m=sqrt(G*M_p/r_m);
KE_m=0.5*M_m*v_m*v_m;
PDCT=(KE_m/KE_p)*(T_p);
printf("Orbital Velocity of Moon: %f m/s \n", v_m);
printf("PlanetDay Characteristic Time: %f seconds \n",
PDCT);
C_m=2*3.14159*r_m;
T_m=C_m/v_m;
Tmoon=T_m*(1.0/24)*(1.0/60)*(1.0/60);
printf("Lunar Orbital Period: %f seconds \n", T_m);
printf("Lunar Orbital Period: %f days \n", Tmoon);
return 0;}}
Now we show running the program (3 examples) for a wide spread of spectral types including F, G, and
K-type stars. We will need to input in the program not just the mass of the star, its luminosity, and size,
but the pressure gradient exponent for the disc from which the star’s planets formed.
To compute the moon’s orbital radius I just use
Where Ag is the molar mass of silver and Au is the molar mass of silver, a connection to the 1.8 that
appears in our Solar System. We use this because we know it works for our Solar System. I compute the
radius of the planet using
But, give the option of putting in your own radius. I have run the program for F5V stars, through GV
stars, to K3V stars and I use this equation to compute the radii of the planets because, again, we know it
works for our star system, and further we found given the way the radius of a star varies with with
luminosity in the HR diagram, this equation always gives a planet around the size of the Earth. I feel this
size is ideal for planets with sophisticated life because of the laws of chemistry determining a functional
density for the planet having water and the right gravity. As such I always use the planet day as one Earth
day, which again I feel is optimal for life in terms of climate. So these values all constant, we only vary
star mass, size, and luminosity as they work on the HR diagram. I also vary the pressure gradient
exponent now using the average theoretical values it has for each spectral class. The trend is that it
steadily decreases on average with mass and luminosity of the star though it can go up and down
depending on the peculiarities of the system. One of the reasons is that while for a G2V star it can range
on average from p= 1.7-2.1, for our Sun, a G2V star, it is actually high, it is 2.5. However, here we will