<p>The expression that is used by NASA/JPL to approximate the relativistic effects on the orbit of a single planet plus the Sun in our solar system is known as the "<a href="https://space.stackexchange.com/a/23409/29864">post-Newtonian expansion</a>" and looks like:</p>

<p><span class="math-container">$$\frac{d\bar{v}}{dt}=-\frac{GM}{r^2}\left(1-\frac{4GM}{rc^2}+\frac{v^2}{c^2}\right)\hat{r} +\frac{4GM}{r^2}\left(\hat{r}\cdot \hat{v}\right)\frac{v^2}{c^2}\hat{v}$$</span></p>

<p>If there are many planets the expression becomes more complex. You can compare this to the classical Newtonian acceleration:</p>

<p><span class="math-container">$$\frac{d\bar{v}}{dt}=-\frac{GM}{r^2}\hat{r}$$</span></p>

<p>I am not a big fan of this approximation but it is what is mostly used.</p>

<hr>

<p>For a pure circular orbit in Schwarzschild coordinates you get the same orbital velocity in GR (in coordinate time) as classically.</p>

<p>I you are dropping an object from rest the initial acceleration in GR (in coordinate time) is the same as classically.</p>

<p>Generally if you want to know if GR or classical Newtonian gravitation results in more acceleration you have to decide if you are interested in the result in "coordinate time" or in "proper time" and the fraction will also vary depending on in what direction the planet is moving as compared to the Sun.</p>

CC BY-SA 4.0
2023-01-14T04:04:31.020Z
Thanks for this PPN formula.  I followed the link but couldnt find the matching NASA/JPL source.  I'm pretty sure that the $-$ and $+$ signs need to be reversed inside the large bracketed term on the RHS of the equation, thus: $(1+\frac{4GM}{rc^2} -\frac{v^2}{c^2})$.  For a circular orbit this term simplifies down to:-  $(1+\frac{3GM}{rc^2})$ since  $v_{circ}^2=\frac{GM}{r}$.
steveOw
CC BY-SA 4.0
2023-01-15T01:16:27.627Z
I found an equation similar to yours:- Eqtn 3.11 in  [
Shahid-Saless, B.; Yeomans, Donald K., 1994, "Relativistic Effects on the Motion of Asteroids and Comets"](https://dataverse.jpl.nasa.gov/dataset.xhtml?persistentId=hdl:2014/32442) .  I still do not understand why the signs (which agree with your eqtn) are as they are and why they seem to be at odds with the "Goldstein-Walter" equations in my question.
steveOw
CC BY-SA 4.0
2023-01-16T21:42:41.410Z
@steveOw The official documentation from the the guys at NASA/JPL is available and presents some outline to a derivation  which is unfortunately beyond me: https://descanso.jpl.nasa.gov/monograph/series2_section.html
Agerhell
CC BY-SA 4.0
2023-01-16T21:57:58.663Z
@steveOw Classically for a circular orbit you must have $GM/r^2 = v^2/r$ (gravity and centrifugal/centripetal acceleration cancels) which leads to $v^2=GM/r$ but you cannot interchange them if you use the NASA/PPN formula.
Agerhell
CC BY-SA 4.0
2023-01-16T22:50:08.373Z
Many thanks for the very useful Descanso link.  I know that strictly I should not take terms from Newtonian to GR/PPN and vice versa without heavy qualification or alteration. But I think that it is legitimate for a broad brush picture of  causes and effects such as the Non Newtonian acceleration of planets and its explanation of the Non-Newtonian apsidal rotation anomalies of Mercury etc.  I am pursuing this problem with a new question here:-https://astronomy.stackexchange.com/questions/51649/problem-with-the-orbital-precession-predicted-by-the-relativistic-acceleration-e
steveOw
CC BY-SA 4.0
2019-05-24T18:30:10.690Z
2019-05-24T18:30:10.690Z
Agerhell
<p>Orbits in Schwarzschild spacetime can be described by the effective potential
$$V_\text{eff} = -\frac{GM}{r} + \frac{\mathfrak{l}^2}{2r^2} - \frac{GM\mathfrak{l}^2}{c^2r^3}\text{,}$$
where $\mathfrak{l} = r^2\dot{\phi}$ is the specific angular momentum of the orbit, which is a conserved quantity. The first two terms match the form of the Newtonian effective potential, except that here we're referring to the Schwarzschild radial coordinate $r$ and proper time of the orbiting particle, instead of radial distance and coordinate time. The first term being the usual gravitational potential and the second being the centrifugal potential, so Goldstein's $V$ does make some sense as a gravitational potential energy term instead.</p>

<p>Therefore, $l^2 = mka(1-e^2)$ with $k = GMm$ means that $l$ is the angular momentum, $l = m\mathfrak{l}$, and
$$\frac{GM\mathfrak{l}^2}{c^2r^3}m = GMm\frac{l^2}{m^2}\frac{1}{c^2r^3} = \underbrace{\frac{kl^2}{m^2c^3}}_b\frac{1}{r^3}\text{,}$$
just as Goldstein says. If we differentiate $\frac{1}{2}m\dot{r}^2 + mV_\text{eff} = \mathcal{E}$ with respect to proper time, then
$$\begin{eqnarray*}m\ddot{r} - \frac{l^2}{mr^3} &amp;=&amp; -\frac{k}{r^2} - \frac{3b}{r^4}\\
&amp;=&amp; -\frac{k}{r^2}\left(1 + 3\frac{l^2}{m^2c^2}\frac{1}{r^2}\right)\\
&amp;=&amp; -\frac{k}{r^2}\left(1 + 3\frac{m(GMm)a(1-e^2)}{m^2c^2}\frac{1}{r^2}\right)\\
&amp;=&amp; -\frac{k}{r^2}\left(1 + 3\frac{v_c^2}{c^2}\frac{a(1-e^2)}{r}\right)\text{.}
\end{eqnarray*}$$
This is dimensionally correct, as both $v_c/c$ and $a/r$ are dimensionless, while
$$\frac{l^2}{mr^3} = \frac{k}{r^2}\frac{a(1-e^2)}{r}\text{.}$$
The left-hand side has the Newtonian form.</p>

CC BY-SA 3.0
2014-10-15T20:44:47.477Z
$\ell$ has dimension $MD^2/T$ due to inclusion of $k=GMm$ in Eqtn 12.50. Maybe Eqtn.12.48 for $b$ should have $m^4$ in denominator rather than $m^2$?
steveOw
CC BY-SA 3.0
2014-10-15T21:18:44.073Z
Aha! I see the error is mine. I confused angular momentum with specific angular momentum (no mass).  Goldstein agrees with Walter. His $\ell^2$ is OK as the second $m$ comes from the term $k=GMm$.
steveOw
CC BY-SA 3.0
2014-10-15T21:24:16.633Z
@steveOw yeah, I misread how the variables were defined too. Eh!
Stan Liou
CC BY-SA 3.0
2014-11-07T16:30:48.647Z
I think your last equation but one should have (a^2/r^2) instead of (a/r) assuming the previous equation is correct. Either way, any presence of r in this term disproves my thesis...which I am now re-evaluating....I may ask a separate question to clarify my thoughts.
steveOw
CC BY-SA 3.0
2014-11-07T17:43:33.583Z
@steveOw Since $l^2/m^2 = GMa(1-e^2)$ as introduced in the beginning of the second paragraph (cf. also [here](https://en.wikipedia.org/wiki/Specific_angular_momentum#Elliptical_orbit) but with $m\ll M$), $a/r$ is correct. But you're very welcome to ask any follow-up questions.
Stan Liou
CC BY-SA 3.0
2014-11-07T18:55:52.763Z
Sorry, I wasn't very clear. I was referring to the change from: $m(GMm)/(m^2r^2)$ to: $v_c^2/r$.  It seems to me that the latter term is missing $a/r$. Which would be valid only for a circular orbit.  BTW I have posted follow-up question [here](https://astronomy.stackexchange.com/questions/7900/can-general-relativity-indicate-phase-dependent-variations-in-planetary-orbital)
steveOw
CC BY-SA 3.0
2014-11-07T21:36:02.557Z
@steveOw but $v_c^2 = GM/r$ already has one factor of $1/r$ in it, so that's why the $1/r^2$ goes to $1/r$, so that's fine too. I'll take a look at your other question, though.
Stan Liou
CC BY-SA 3.0
2014-11-08T18:01:54.707Z
Ah, that explains the discrepancy, I was assuming $v_c^2 = GM/a$.  Walter assumes a near circular orbit so $r \approx a$ and $a(1-e^2)/r \approx 1$.  In your penultimate formula RHS inside brackets can be expressed $ 1 + 3h^2/c^2r^2$ = $1+3v_T^2/c^2$ where v_T is the instantaneous transverse velocity. Which (I now see) answers my follow-on question. (I will look at your separate answer there for completeness).
steveOw
CC BY-SA 3.0
2014-10-15T17:50:55.947Z
2014-10-15T21:23:12.217Z
2014-10-15T21:23:12.217Z
Stan Liou
<p>For a hypothetical orbital system (Sun + single planet) the Newtonian model and the General Relativity (GR) model produce different expressions for the gravitational effect of the Sun on the planet. This is well known.</p>

<p>The ratio between the Newtonian and GR effects is expressed in different ways by different writers.</p>

<p>I am having trouble reconciling two such expressions of the Newtonian:GR ratio.</p>

<p>Firstly <a href="http://books.google.co.uk/books?id=V4_s91-Vun4C&amp;pg=PA482&amp;lpg=PA482&amp;dq=we+recall+from+section+7.6.1&amp;source=bl&amp;ots=RyU1Adp8h7&amp;sig=qQ5_KyjoDhaSaOadgP8zyy8ubIc&amp;hl=en&amp;sa=X&amp;ei=Hlc-VJDJK9TzaoHlgKgL&amp;ved=0CCEQ6AEwAA#v=onepage&amp;q=we%20recall%20from%20section%207.6.1&amp;f=false" rel="nofollow">Walter (2008)</a> (equation 12.7.6, page 482) presents  the following expression for the equation of motion produced from the GR model</p>

<p>$$\frac{d^2\,u}{d\theta^2} + u = \frac{GM}{h^2} + \frac{3GM}{c^2}u^2$$
where $u= (1/r)$, $h=vr$, $G$ is the universal constant of gravitation, $M$ is mass of the Sun, $c$ is speed of light.  Here the term $GM/h^2$ is the ordinary Newtonian term and the term $3GMu^2/c^2$ is the additional term introduced by GR.
<p>From this Walter derives the approximate ratio between Newtonian and GR effects as
$(1)$ to $(1 + 3v^2/c^2)$ where $v = \sqrt{GM/r}$ is the orbital speed of the planet in a circular orbit (with distance $r$ = $a$, the semi-major axis).</p>

<p>Secondly, an alternative presentation (referring to the so-called Schwartzchild solution) is given by Goldstein in <a href="http://rads.stackoverflow.com/amzn/click/0201657023" rel="nofollow">Classical Mechanics (3rd Edition)</a> pages 536-538.  The GR potential $V_{GR}$ is given by
$$V = -\frac{GMm}{r} -\frac{b}{r^3}$$
where $m$ is the target body mass and $b$ is a constant (Goldstein uses $h$ instead of $b$, see below, but I have already used $h$ to mean something different in Walter above,)
<p> differentiating the potential with respect to distance $r$ to give force we derive
$$F_{GR} = \frac{GMm}{r^2} + \frac{3b}{r^4}$$
<p>Now Goldstein defines the constant $b$ thus :-
$$
b = \frac{k\,l^2}{m^2c^2} \qquad\text{ Goldstein eqtn [12.48]} 
$$
where
$$
k=GMm 
$$
and 
$$
l^2 = mka(1-e^2) \qquad\text{ Goldstein eqtn[12.50]}
$$</p>

<p>So</p>

<p>$$b = \frac{GMm\, m\, GMm\, a(1-e^2)}{m^2c^2}
= \frac{GMm \, L^2}{c^2}
= \frac{GMm \,m^2 v_c^2 a^2}{c^2}
$$</p>

<p>So the GR force equation becomes
$$
F_{GR} = \frac{GMm}{r^2} + \frac{3GMm m^2 v_c^2 a^2}{r^4c^2}
$$
substituting $a$ by $r$ we get
$$
F_{GR} = \frac{GMm}{r^2} + \frac{3GMm m^2 v_c^2}{r^2c^2}
= \frac{GMm}{r^2} \left( 1 + \frac{3 v_c^2 \, m^2}{c^2} \right)
$$</p>

<p>So the Newtonian:GR ratio derived from Goldstein is the same as the ratio derived by Walter except that the former has the additional term of $m^2$ in the numerator.
Even if we tried to fudge this numerically by invoking a unit mass target, it would still be dimensionally incorrect.
<p> So what is the correct ratio?
$$$$
<p>UPDATE ---------------------------------------------------------------------
<p>In the refactoring of $b$ I used angular momentum $L$ when I should have used specific angular momentum $\mathfrak{l}$. After correction the extra $m^2$ disappears. Goldstein agrees with Walter. My thanks to Stan Liou for illumination.
<p>Corrected analysis:-
$$b = \frac{GMm\, m\, GMm\, a(1-e^2)}{m^2c^2}
= \frac{GMm \, \mathfrak{l}^2}{c^2}
= \frac{GMm \,v_c^2 a^2}{c^2}
$$</p>

<p>So the GR force equation becomes
$$
F_{GR} = \frac{GMm}{r^2} + \frac{3GMm v_c^2 a^2}{r^4c^2}
$$
substituting $a$ by $r$ we get
$$
F_{GR} = \frac{GMm}{r^2} + \frac{3GMm v_c^2}{r^2c^2}
= \frac{GMm}{r^2} \left( 1 + \frac{3 v_c^2}{c^2} \right)
$$</p>

<p>So the correct ratio of Newtonian to GR gravitational force is:-
$$
F_{Newtonian}:F_{GR}
\approx  1: \left( 1 + \frac{3 v_c^2}{c^2} \right)
$$</p>

<p>NOTES</p>

<p>This ratio is approximate and only applies in the "low velocity, weak field" sub-domain of the GR model.  </p>

<p>Goldstein also emphasises that the GR effect is not a velocity effect (presumably as in the velocity of the target body through any kind of aether or flux).</p>

<p>Coincidentally (in the same sub-domain e.g. Mercury orbitting the Sun) a modified Newtonian radial force of magnitude $f=GMm/r^2 * [1 + 3v_t^2/c^2]$, where $v_t$ is the instantaneous transverse velocity of a small target planet, produces non-Newtonian apsidal rotation ("perihelion precession") of the same magnitude (within 1%) as GR.  </p>

<p>Goldstein needs to be read with care. Here he uses $l$ to denote angular momentum elsewhere (e.g. eqtn [1.7]) he uses $L$. He often refers to $V$ as "potential" when he is clearly referring to "potential energy" (e.g. eqtn [3.49]).</p>

CC BY-SA 3.0
2014-10-16T11:53:35.937Z
There is no one specific "ratio". If that's all there was to general relativity, GR would be easy. GR is not "easy". The relationship posted in this question is perhaps the simplest of simple linearizations of general relativity.
David Hammen
CC BY-SA 3.0
2014-10-16T14:46:21.780Z
David is of course correct in that this kind of comparison only makes sense for slow orbits in a weak-field approximation, though fortunately that's also the context of this question. It may be noted that for the specific case of Schwarzschild spacetime, orbits are *exactly* described by the effective potential; the approximation comes in when one treats the radial coordinate and proper time as if they were Newtonian, which is invalid in more general situations.
Stan Liou
CC BY-SA 3.0
2014-10-17T15:26:18.233Z
David & Stan: Thanks. Yes I was aware but have added clarification at end of the Question.
steveOw
<orbit><general-relativity>
What is the correct ratio of Newtonian to General Relativistic gravitational effects for Sun + single planet orbital system
steveOw
# What is the correct ratio of Newtonian to General Relativistic gravitational effects for Sun + single planet orbital system

(Asked by: username_0 on 2014-10-15)

For a hypothetical orbital system (Sun + single planet) the Newtonian model and the General Relativity (GR) model produce different expressions for the gravitational effect of the Sun on the planet. This is well known.

The ratio between the Newtonian and GR effects is expressed in different ways by different writers.

I am having trouble reconciling two such expressions of the Newtonian:GR ratio.

Firstly [Walter (2008)](http://books.google.co.uk/books?id=V4_s91-Vun4C&pg=PA482&lpg=PA482&dq=we+recall+from+section+7.6.1&source=bl&ots=RyU1Adp8h7&sig=qQ5_KyjoDhaSaOadgP8zyy8ubIc&hl=en&sa=X&ei=Hlc-VJDJK9TzaoHlgKgL&ved=0CCEQ6AEwAA#v=onepage&q=we%20recall%20from%20section%207.6.1&f=false) (equation 12.7.6, page 482) presents the following expression for the equation of motion produced from the GR model

$$\frac{d^2\,u}{d\theta^2} + u = \frac{GM}{h^2} + \frac{3GM}{c^2}u^2$$
where $u= (1/r)$, $h=vr$, $G$ is the universal constant of gravitation, $M$ is mass of the Sun, $c$ is speed of light. Here the term $GM/h^2$ is the ordinary Newtonian term and the term $3GMu^2/c^2$ is the additional term introduced by GR.

From this Walter derives the approximate ratio between Newtonian and GR effects as
$(1)$ to $(1 + 3v^2/c^2)$ where $v = \sqrt{GM/r}$ is the orbital speed of the planet in a circular orbit (with distance $r$ = $a$, the semi-major axis).

Secondly, an alternative presentation (referring to the so-called Schwartzchild solution) is given by Goldstein in [Classical Mechanics (3rd Edition)](http://rads.stackoverflow.com/amzn/click/0201657023) pages 536-538. The GR potential $V\_{GR}$ is given by
$$V = -\frac{GMm}{r} -\frac{b}{r^3}$$
where $m$ is the target body mass and $b$ is a constant (Goldstein uses $h$ instead of $b$, see below, but I have already used $h$ to mean something different in Walter above,)

differentiating the potential with respect to distance $r$ to give force we derive
$$F\_{GR} = \frac{GMm}{r^2} + \frac{3b}{r^4}$$

Now Goldstein defines the constant $b$ thus :-
$$
b = \frac{k\,l^2}{m^2c^2} \qquad\text{ Goldstein eqtn [12.48]}
$$
where
$$
k=GMm
$$
and
$$
l^2 = mka(1-e^2) \qquad\text{ Goldstein eqtn[12.50]}
$$

So

$$b = \frac{GMm\, m\, GMm\, a(1-e^2)}{m^2c^2}
= \frac{GMm \, L^2}{c^2}
= \frac{GMm \,m^2 v\_c^2 a^2}{c^2}
$$

So the GR force equation becomes
$$
F\_{GR} = \frac{GMm}{r^2} + \frac{3GMm m^2 v\_c^2 a^2}{r^4c^2}
$$
substituting $a$ by $r$ we get
$$
F\_{GR} = \frac{GMm}{r^2} + \frac{3GMm m^2 v\_c^2}{r^2c^2}
= \frac{GMm}{r^2} \left( 1 + \frac{3 v\_c^2 \, m^2}{c^2} \right)
$$

So the Newtonian:GR ratio derived from Goldstein is the same as the ratio derived by Walter except that the former has the additional term of $m^2$ in the numerator.
Even if we tried to fudge this numerically by invoking a unit mass target, it would still be dimensionally incorrect.

So what is the correct ratio?
$$$$

UPDATE ---------------------------------------------------------------------

In the refactoring of $b$ I used angular momentum $L$ when I should have used specific angular momentum $\mathfrak{l}$. After correction the extra $m^2$ disappears. Goldstein agrees with Walter. My thanks to Stan Liou for illumination.

Corrected analysis:-
$$b = \frac{GMm\, m\, GMm\, a(1-e^2)}{m^2c^2}
= \frac{GMm \, \mathfrak{l}^2}{c^2}
= \frac{GMm \,v\_c^2 a^2}{c^2}
$$

So the GR force equation becomes
$$
F\_{GR} = \frac{GMm}{r^2} + \frac{3GMm v\_c^2 a^2}{r^4c^2}
$$
substituting $a$ by $r$ we get
$$
F\_{GR} = \frac{GMm}{r^2} + \frac{3GMm v\_c^2}{r^2c^2}
= \frac{GMm}{r^2} \left( 1 + \frac{3 v\_c^2}{c^2} \right)
$$

So the correct ratio of Newtonian to GR gravitational force is:-
$$
F\_{Newtonian}:F\_{GR}
\approx 1: \left( 1 + \frac{3 v\_c^2}{c^2} \right)
$$

NOTES

This ratio is approximate and only applies in the "low velocity, weak field" sub-domain of the GR model.

Goldstein also emphasises that the GR effect is not a velocity effect (presumably as in the velocity of the target body through any kind of aether or flux).

Coincidentally (in the same sub-domain e.g. Mercury orbitting the Sun) a modified Newtonian radial force of magnitude $f=GMm/r^2 \* [1 + 3v\_t^2/c^2]$, where $v\_t$ is the instantaneous transverse velocity of a small target planet, produces non-Newtonian apsidal rotation ("perihelion precession") of the same magnitude (within 1%) as GR.

Goldstein needs to be read with care. Here he uses $l$ to denote angular momentum elsewhere (e.g. eqtn [1.7]) he uses $L$. He often refers to $V$ as "potential" when he is clearly referring to "potential energy" (e.g. eqtn [3.49]).

**Tags:** orbit, general-relativity
> **Comments:**
> **username_1**: There is no one specific "ratio". If that's all there was to general relativity, GR would be easy. GR is not "easy". The relationship posted in this question is perhaps the simplest of simple linearizations of general relativity.  
> **username_2**: David is of course correct in that this kind of comparison only makes sense for slow orbits in a weak-field approximation, though fortunately that's also the context of this question. It may be noted that for the specific case of Schwarzschild spacetime, orbits are *exactly* described by the effective potential; the approximation comes in when one treats the radial coordinate and proper time as if they were Newtonian, which is invalid in more general situations.  
> **username_0**: David & Stan: Thanks. Yes I was aware but have added clarification at end of the Question.  

---

## 2 answers

### Answer by username_2 on 2014-10-15. Score: 6 | Accepted answer

Orbits in Schwarzschild spacetime can be described by the effective potential
$$V\_\text{eff} = -\frac{GM}{r} + \frac{\mathfrak{l}^2}{2r^2} - \frac{GM\mathfrak{l}^2}{c^2r^3}\text{,}$$
where $\mathfrak{l} = r^2\dot{\phi}$ is the specific angular momentum of the orbit, which is a conserved quantity. The first two terms match the form of the Newtonian effective potential, except that here we're referring to the Schwarzschild radial coordinate $r$ and proper time of the orbiting particle, instead of radial distance and coordinate time. The first term being the usual gravitational potential and the second being the centrifugal potential, so Goldstein's $V$ does make some sense as a gravitational potential energy term instead.

Therefore, $l^2 = mka(1-e^2)$ with $k = GMm$ means that $l$ is the angular momentum, $l = m\mathfrak{l}$, and
$$\frac{GM\mathfrak{l}^2}{c^2r^3}m = GMm\frac{l^2}{m^2}\frac{1}{c^2r^3} = \underbrace{\frac{kl^2}{m^2c^3}}\_b\frac{1}{r^3}\text{,}$$
just as Goldstein says. If we differentiate $\frac{1}{2}m\dot{r}^2 + mV\_\text{eff} = \mathcal{E}$ with respect to proper time, then
$$\begin{eqnarray\*}m\ddot{r} - \frac{l^2}{mr^3} &=& -\frac{k}{r^2} - \frac{3b}{r^4}\\
&=& -\frac{k}{r^2}\left(1 + 3\frac{l^2}{m^2c^2}\frac{1}{r^2}\right)\\
&=& -\frac{k}{r^2}\left(1 + 3\frac{m(GMm)a(1-e^2)}{m^2c^2}\frac{1}{r^2}\right)\\
&=& -\frac{k}{r^2}\left(1 + 3\frac{v\_c^2}{c^2}\frac{a(1-e^2)}{r}\right)\text{.}
\end{eqnarray\*}$$
This is dimensionally correct, as both $v\_c/c$ and $a/r$ are dimensionless, while
$$\frac{l^2}{mr^3} = \frac{k}{r^2}\frac{a(1-e^2)}{r}\text{.}$$
The left-hand side has the Newtonian form.

> **Comments:**
> **username_0**: $\ell$ has dimension $MD^2/T$ due to inclusion of $k=GMm$ in Eqtn 12.50. Maybe Eqtn.12.48 for $b$ should have $m^4$ in denominator rather than $m^2$?  
> **username_0**: Aha! I see the error is mine. I confused angular momentum with specific angular momentum (no mass).  Goldstein agrees with Walter. His $\ell^2$ is OK as the second $m$ comes from the term $k=GMm$.  
> **username_2**: @steveOw yeah, I misread how the variables were defined too. Eh!  
> **username_0**: I think your last equation but one should have (a^2/r^2) instead of (a/r) assuming the previous equation is correct. Either way, any presence of r in this term disproves my thesis...which I am now re-evaluating....I may ask a separate question to clarify my thoughts.  
> **username_2**: @steveOw Since $l^2/m^2 = GMa(1-e^2)$ as introduced in the beginning of the second paragraph (cf. also [here](https://en.wikipedia.org/wiki/Specific_angular_momentum#Elliptical_orbit) but with $m\ll M$), $a/r$ is correct. But you're very welcome to ask any follow-up questions.  
> **username_0**: Sorry, I wasn't very clear. I was referring to the change from: $m(GMm)/(m^2r^2)$ to: $v_c^2/r$.  It seems to me that the latter term is missing $a/r$. Which would be valid only for a circular orbit.  BTW I have posted follow-up question [here](https://astronomy.stackexchange.com/questions/7900/can-general-relativity-indicate-phase-dependent-variations-in-planetary-orbital)  
> **username_2**: @steveOw but $v_c^2 = GM/r$ already has one factor of $1/r$ in it, so that's why the $1/r^2$ goes to $1/r$, so that's fine too. I'll take a look at your other question, though.  
> **username_0**: Ah, that explains the discrepancy, I was assuming $v_c^2 = GM/a$.  Walter assumes a near circular orbit so $r \approx a$ and $a(1-e^2)/r \approx 1$.  In your penultimate formula RHS inside brackets can be expressed $ 1 + 3h^2/c^2r^2$ = $1+3v_T^2/c^2$ where v_T is the instantaneous transverse velocity. Which (I now see) answers my follow-on question. (I will look at your separate answer there for completeness).  

---

### Answer by username_3 on 2019-05-24. Score: 2

The expression that is used by NASA/JPL to approximate the relativistic effects on the orbit of a single planet plus the Sun in our solar system is known as the "[post-Newtonian expansion](https://space.stackexchange.com/a/23409/29864)" and looks like:

$$\frac{d\bar{v}}{dt}=-\frac{GM}{r^2}\left(1-\frac{4GM}{rc^2}+\frac{v^2}{c^2}\right)\hat{r} +\frac{4GM}{r^2}\left(\hat{r}\cdot \hat{v}\right)\frac{v^2}{c^2}\hat{v}$$

If there are many planets the expression becomes more complex. You can compare this to the classical Newtonian acceleration:

$$\frac{d\bar{v}}{dt}=-\frac{GM}{r^2}\hat{r}$$

I am not a big fan of this approximation but it is what is mostly used.

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For a pure circular orbit in Schwarzschild coordinates you get the same orbital velocity in GR (in coordinate time) as classically.

I you are dropping an object from rest the initial acceleration in GR (in coordinate time) is the same as classically.

Generally if you want to know if GR or classical Newtonian gravitation results in more acceleration you have to decide if you are interested in the result in "coordinate time" or in "proper time" and the fraction will also vary depending on in what direction the planet is moving as compared to the Sun.

> **Comments:**
> **username_0**: Thanks for this PPN formula.  I followed the link but couldnt find the matching NASA/JPL source.  I'm pretty sure that the $-$ and $+$ signs need to be reversed inside the large bracketed term on the RHS of the equation, thus: $(1+\frac{4GM}{rc^2} -\frac{v^2}{c^2})$.  For a circular orbit this term simplifies down to:-  $(1+\frac{3GM}{rc^2})$ since  $v_{circ}^2=\frac{GM}{r}$.  
> **username_0**: I found an equation similar to yours:- Eqtn 3.11 in  [ Shahid-Saless, B.; Yeomans, Donald K., 1994, "Relativistic Effects on the Motion of Asteroids and Comets"](https://dataverse.jpl.nasa.gov/dataset.xhtml?persistentId=hdl:2014/32442) .  I still do not understand why the signs (which agree with your eqtn) are as they are and why they seem to be at odds with the "Goldstein-Walter" equations in my question.  
> **username_3**: @steveOw The official documentation from the the guys at NASA/JPL is available and presents some outline to a derivation  which is unfortunately beyond me: https://descanso.jpl.nasa.gov/monograph/series2_section.html  
> **username_3**: @steveOw Classically for a circular orbit you must have $GM/r^2 = v^2/r$ (gravity and centrifugal/centripetal acceleration cancels) which leads to $v^2=GM/r$ but you cannot interchange them if you use the NASA/PPN formula.  
> **username_0**: Many thanks for the very useful Descanso link.  I know that strictly I should not take terms from Newtonian to GR/PPN and vice versa without heavy qualification or alteration. But I think that it is legitimate for a broad brush picture of  causes and effects such as the Non Newtonian acceleration of planets and its explanation of the Non-Newtonian apsidal rotation anomalies of Mercury etc.  I am pursuing this problem with a new question here:-https://astronomy.stackexchange.com/questions/51649/problem-with-the-orbital-precession-predicted-by-the-relativistic-acceleration-e  

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