User:Mark Widmer/sandbox

Sandbox. Mark Widmer (talk) 01:17, 5 August 2021 (UTC)

Heat equation

Heat_equation

Define variables when equation is used for temperature: u=temperature, k = k_therm / (c*rho)

Define variable when equation refers to diffusion: u = density???

Draft for additions to Hill_sphere New sections:

Hill sphere and L1 Lagrange point

-- added note in Formulas section

Hill sphere of the Sun

-- added to article

Hill sphere of objects that orbit Earth

The Moon -- added to article

Artificial satellites in low-Earth orbit -- added to article

L1 Lagrange point for comparable-mass objects

Usually, derivations of the L1 point assume a planetary mass that is much less than the star's mass. This no longer applies if the orbiting objects have comparable masses. This is the case for many binary star systems. For example, in the Alpha Centauri system, the stars Alpha Centauri A and B have masses that are 1.1 and 0.9 times that of the Sun, respectively, or a mass ratio of about 0.8.

For two equal-mass objects, let R be the distance between the objects. Each object is then in a circular orbit of radius R/2 about the center of mass, which is halfway between them.

Outline:

We follow the derivation for small planet/star mass ratio given at http://www.phy6.org/stargaze/Slagrang.htm, without making the small-ratio approximations that are incorporated there.

Planet/star mass ratio $\mu =m/M$, with $0<\mu <=1$

Equate the gravitational force (which acts at a distance R) with the centripetal force (for a circle of radius $R/(1+\mu )$):

${\frac {GmM}{R^{2}}}={\frac {mv^{2}}{\frac {R}{1+\mu }}}={\frac {mv^{2}(1+\mu )}{R}}$

Mult by R/m:

${\frac {GM}{R}}=(1+\mu )v^{2}$

Substitute for $v={\frac {2\pi {\frac {R}{1+\mu }}}{T}}$

${\frac {GM}{R}}={\frac {(1+\mu )4\pi ^{2}R^{2}}{T^{2}(1+\mu )^{2}}}$

${\frac {GM}{R^{3}}}={\frac {4\pi ^{2}}{T^{2}(1+\mu )}}$

${\frac {GM}{R^{3}}}={\frac {4\pi ^{2}}{(1+\mu )T^{2}}}$

An small-mass object at the L1 point, a distance r from object m, will have an orbit with radius ${\frac {R}{1+\mu }}-r$ and the same period T:

${\frac {GM}{(R-r)^{2}}}-{\frac {Gm}{r^{2}}}={\frac {v^{2}}{{\frac {R}{1+\mu }}-r}}$

$v={\frac {2\pi ({\frac {R}{1+\mu }}-r)}{T}}$,

so

${\frac {GM}{(R-r)^{2}}}-{\frac {Gm}{r^{2}}}={\frac {4\pi ^{2}({\frac {R}{1+\mu }}-r)^{2}}{T^{2}}}{\frac {1}{{\frac {R}{1+\mu }}-r}}={\frac {4\pi ^{2}({\frac {R}{1+\mu }}-r)}{T^{2}}}$

Since T is the same for the planet and an object at the L1 point,

${\frac {4\pi ^{2}}{T^{2}}}={\frac {GM(1+\mu )}{R^{3}}}={\frac {GM}{(R-r)^{2}({\frac {R}{1+\mu }}-r)}}-{\frac {Gm}{r^{2}({\frac {R}{1+\mu }}-r)}}$

Divide through by GM

${\frac {(1+\mu )}{R^{3}}}={\frac {1}{(R-r)^{2}({\frac {R}{1+\mu }}-r)}}-{\frac {\mu }{r^{2}({\frac {R}{1+\mu }}-r)}}$

${\frac {(1+\mu )}{R^{3}}}({\frac {R}{1+\mu }}-r)={\frac {1}{(R-r)^{2}}}-{\frac {\mu }{r^{2}}}$

${\frac {R-r(1+\mu )}{R^{3}}}={\frac {1}{(R-r)^{2}}}-{\frac {\mu }{r^{2})}}$

${\frac {R-r(1+\mu )}{R}}{\frac {(R-r)^{2}}{R^{2}}}=1-{\frac {\mu (R-r)^{2}}{r^{2}}}$

$(1-\rho (1+\mu ))(1-\rho )^{2}=1-\mu ({\frac {1}{\rho }}-1)^{2}$

$\rho ^{2}(1-\rho (1+\mu ))(1-\rho )^{2}=\rho ^{2}-\mu (1-\rho )^{2}$

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${\frac {1}{R}}={\frac {1}{T}}$

${\frac {1}{r}}$

$\alpha \beta \gamma \Delta \theta \pi$

$\omega {\mbox{ is }}2\pi f$

$\omega \mathrm {is} 2\pi f$

${\displaystyle }$

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