GR Lagrangian Part 2 Homework Statement Solution

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SUMMARY

The discussion focuses on solving the second-order correction to the gravitational field ##h## in the context of Einstein gravity using the Lagrangian density $$L=-\frac{1}{2}h\Box h + (M_p)^ah^2\Box h - (M_p)^b h T$$. The equations of motion derived from this Lagrangian lead to $$\Box h = (M_p)^{a}\Box(h^2)-(M_p)^bT$$. The user attempts to find the second-order solution for ##h##, denoting it as ##h_1##, and questions the validity of discarding the function ##f(x)## in the equation. The user also notes a discrepancy in the expected magnitude of the second-order correction ##h_1## compared to the first-order approximation ##h_0##, indicating a misunderstanding in the calculations.

PREREQUISITES
  • Understanding of Lagrangian mechanics in the context of General Relativity.
  • Familiarity with the Einstein field equations and their implications.
  • Knowledge of Quantum Field Theory (QFT) principles.
  • Basic concepts of perturbation theory in gravitational fields.
NEXT STEPS
  • Review the derivation of the Einstein field equations and their applications in gravitational physics.
  • Study perturbation theory in General Relativity to clarify the treatment of higher-order corrections.
  • Examine the role of the function ##f(x)## in the context of wave equations and boundary conditions.
  • Learn about the implications of second-order corrections in gravitational interactions, particularly in orbital mechanics.
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Students and researchers in theoretical physics, particularly those focusing on General Relativity and Quantum Field Theory, as well as anyone involved in advanced gravitational studies and orbital mechanics.

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Homework Statement


This is a continuation of this problem. I will rewrite it here too:
The Lagrangian density for the ##h=h^{00}## term of the Einstein gravity tensor can be simplified to: $$L=-\frac{1}{2}h\Box h + (M_p)^ah^2\Box h - (M_p)^b h T$$ The equations of motion following from this Lagrangian looks roughly like (I didn't calculate this, they are given in the problem): $$\Box h = (M_p)^{a}\Box(h^2)-(M_p)^bT$$ For a point source ##T=m\delta^3(x)##, solve the equation for h to second order in the source T, with ##M_p=\frac{1}{\sqrt{G_N}}## and calculate the correction to the Mercury angular frequency orbit around the sun compared to the first order approximation.

Homework Equations

The Attempt at a Solution


Continuing the same logic as before I write $$h=h_0+h_1+h_2...$$ where ##h_0## is first order in T, ##h_1## is second order and so on. Before, I got for the first order $$h_0=-\frac{M_p^b m }{4 \pi r}$$ Now if we go to the second order, the equation we need to solve is: $$\Box h_1 = (M_p)^a\Box(h_0^2)$$ which is equivalent to $$\Box (h_1 - (M_p)^a h_0^2) = 0$$ $$h_1 = (M_p)^a h_0^2 + f(x)$$ where ##f(x)## is such that ##\Box f = \nabla f = 0## (I replaced ##\Box## with ##\nabla## as the source is time independent). Is it ok up to now? Now first thing I am confused about, can I discard this ##f##? in the equation of motion it seems like ##h## appear with ##\Box## so I think f will not affect the equations, but I am not 100% sure this is true. Now for the orbit, to first order I used $$m_{Mercury}\omega^2 r = \frac{m_{Mercury}}{M_p}(-\nabla h_0)$$ where that ##M_p## comes from the normalization (as I was told in the first post). And from here I got the first order approximation for ##\omega##. For the second order, I tried the same thing (this is QFT class, so I don't think I am expected to use GR, and they ask for a rough approximation, anyway) $$m_{Mercury}\omega^2 r = \frac{m_{Mercury}}{M_p}(-\nabla (h_0+h_1))$$ However something is wrong as the correction should be very small, however, ##h_1## going like ##h_0^2##, contains ##m^2## which here m is the mass of the sun so overall, the value of ##h_1## is bigger than ##h_0## which doesn't make sense for a second order correction. What is wrong with my calculations? Thank you!
 
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Since ##h_0 \ll 1##, clearly ##h_0^2 \ll h_0##.
 

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