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What is the observed precession of Mercury?

  1. Nov 19, 2011 #1
    The precession of Mercury is presented as one of the threshold moments for general relativity. Are there any publicly available summaries of the classical anomaly? Most refer to a 1947 paper that uses an outdated reference frame.

    Clemence, G. M. (1947). "The Relativity Effect in Planetary Motions". Reviews of Modern Physics 19 (4): 361–364.

    This source gives a precession of the equinoxes of 5025.64, an observed precession of 5599.74 and a tug from the planets of 531.63. This produces an actual precession of 574.1.

    NASA gives a value of 5028.83 for the precession of the equinox, using a modern standard frame. Is there a publicly reference for the actual precession of Mercury, or the precession in J2000 used by NASA?

    http://ssd.jpl.nasa.gov/?constants

    This source from 2008 gives an observed precession of 5600.73, but is unclear what frame is used.

    http://books.google.com/books?id=fp9wrkMYHvMC&pg=PA70#v=onepage&q&f=false

    Is it inaccurate to conclude the current values suggest a classical anomaly as follows:

    The precession of Mercury is [itex]5600.73-5028.83-531.63=40.27[/itex], a 2.71 arcsec/century variance from the 42.98 prediction of GR.
     
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  3. Nov 20, 2011 #2

    D H

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    Yes, it is inaccurate to conclude that.
     
  4. Nov 20, 2011 #3
    Ok. I was assuming it was inaccurate to conclude that.

    I was wanting to know where the error in the calculation came from, and how that error can be expressed using data no older than 1990, except for the perturbative effects like the tug from the planets and the oblateness of the sun.

    I have found this link, giving a precession of the equinoxes of 5028.7955[itex]\pm[/itex]0.0003.

    http://iopscience.iop.org/1538-3881/126/1/494/fulltext

    The effect from the oblateness of the sun is given as 0.0245

    When I use the error measures listed at the sources I provided get that the uncertainty in the excess precession of [itex]2.70\pm0.80[/itex] after the GR correction of 42.98 is made.

    Where is the current data showing this calculation to be in error?
     
  5. Nov 20, 2011 #4

    atyy

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    Maybe try the discussion in section 3.5 of http://relativity.livingreviews.org/Articles/lrr-2006-3/ [Broken]? Will gives a reference [238] published in 1990 which is Shapiro, I.I., “Solar system tests of general relativity: Recent results and present plans” in Proceedings of the 12th International Conference on General Relativity and Gravitation, unfortunately probably not freely available.
     
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  6. Nov 20, 2011 #5

    D H

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    I just told you you cannot do that. So why do you persist?

    There is no current data. It is a solved problem. The most recent publication was R.L.Duncombe, Astronomical Journal, 61:174 (1956). That (not Clemence) is the source of the numbers in the text you cited.

    Since then, advances in computation have enabled a switch in focus from the orbital element approach of the 1800s to numerical techniques. Astronomers, along with mission planners at various space agencies, do not need and do not precession to predict the position of the planets.
     
  7. Nov 20, 2011 #6

    DaveC426913

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    All you acceded to was that his conclusion was inaccurate. You were silent about what step(s) leading up to it you were referring to, forcing him to zero in on the flaw in his logic.
     
  8. Nov 20, 2011 #7

    D H

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    The problem is he is using the precession of the equinoxes as expressed in ICRF but is keeping the observed precession of Mercury in whatever frame was used by Clemence. That is downright invalid.

    Modern tests of general relativity will almost invariably be in the form of a parameterized post Newtonian formalism. There is plenty of recent data on these kinds of tests.
     
  9. Nov 20, 2011 #8
    Hmm, why is that actually necessary, any powerful computer can numerically solve integrals right?
     
  10. Nov 20, 2011 #9

    D H

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    Most, if not all, of these PPN tests would not be possible without the use of modern computers.
     
  11. Nov 20, 2011 #10
    You are not answering my question.
     
  12. Nov 20, 2011 #11

    D H

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    What integrals are you talking about, and what does your question have to do with this thread?
     
  13. Nov 20, 2011 #12
    I am not sure what is so difficult in understanding what I ask.

    You claim that GR tests will almost invariably be in the form of a parameterized post Newtonian formalism.

    I ask why? Is that perhaps not allowed here?

    Or more specific why do you believe that the Perihelion Advance must be solved using PPN?

    In GR we can describe Mercury's orbit using a simple differential equation or an integral as we can approximate it as a test particle in a Schwarschild solution with the Sun as the central mass.

    So why not use that? Frankly I do not see any reason why we would need PPN for this.
    So that's why I ask do I perhaps miss something?
     
    Last edited: Nov 20, 2011
  14. Nov 20, 2011 #13

    atyy

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    The PPN parameters predicted by GR are known. The PPN parameters are used for convenience so that everyone uses the same language - the current PPN parameters evolved from several earlier slightly different PPN formalisms. GR can be placed in PPN form only for weak gravity.

    The Will review linked to above says "Of course, some systems cannot be properly described by any post-Newtonian approximation because their behavior is fundamentally controlled by strong gravity. These include the imploding cores of supernovae, the final merger of two compact objects, the quasinormal-mode vibrations of neutron stars and black holes, the structure of rapidly rotating neutron stars, and so on. Phenomena such as these must be analyzed using different techniques. Chief among these is the full solution of Einstein’s equations via numerical methods. This field of “numerical relativity” is a rapidly growing and maturing branch of gravitational physics ..."
     
  15. Nov 20, 2011 #14

    D H

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    Several reasons. Just a few are that it provides

    - A lingua franca by which different tests of GR can be compared. It turns out that there are far stronger tests of GR than the precession of Mercury.

    - A way to combine disparate tests. A given model of gravitation might pass a slew of individual tests but could fail when those tests are jointly combined in the PPN parameter space. So far GR has passed all such meta-analyses.

    - The ability to test not only GR but also to test (and compare) alternative formulations of gravitation.


    I never said that; so please stop putting words in my mouth. That is however exactly how perihelion advance is oftentimes calculated.

    You are missing

    - The influence of the other planets, which are an order of magnitude larger than that of general relativity.

    - That orbital elements provide a very nice way to visualize orbits but not so nice way to calculate orbits. The tweaks to Keplerian orbits needed to make them accurate get downright ugly.

    - That the precession of Mercury is essentially a solved problem. It is a comparatively weak test of relativity. Modern physics relies on much stricter tests of GR.

    - That the PPN formalism generalizes to encompass alternative formulations of gravitation other than GR.
     
  16. Nov 20, 2011 #15
    I am not missing that at all.

    So are you claiming that the influence of other planets is actually modeled by using GR as opposed to only the perihelion shift? I think the 'other planets' part it is copied verbatim from Newtonian theory with the argument (which I do not claim is wrong) that the difference is negligible. Do you think I am wrong about that? I so, please provide a reference to a calculation where the planetary influences are taken into account using GR.

    I guess then we have to argue what the word ugly means scientifically.

    I think we can calculate Schwarzschild orbits very easily with a decent size desktop and a good math program. If we take some valid initial conditions where the perihelion is at a given coordinate location we can then solve the equation to get the next location after one orbit. Then we get the GR part and leave the extra planetary influences as 'similar to Newton'.

    You think I am wrong about that?
     
    Last edited: Nov 20, 2011
  17. Nov 20, 2011 #16

    D H

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    That is exactly what you will do if you follow the recommendations of the International Astronomical Union and wish to keep up with the Joneses (The Institute of Applied Astronomy, The Paris Observatory, and JPL) of the solar system modeling world.

    Pitjeva, E.V., "EPM ephemerides and relativity," Proceedings of the International Astronomical Union (2009), 5 : pp 170-178
    http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=6911132
    All the modern ephemerides: DE – JPL (Folkner et al., 2008), EPM – IAA RAS (Pitjeva, 2009), INPOP – IMCCE (Fienga et al., 2008) are based upon relativistic equation of motion for celestial bodies and light rays as well as relativistic time scales. The numerical integration of the equations of celestial bodies motion has been performed in the Parameterized Post–Newtonian metric for General Relativity in the TDB time scale; the relativistic effects of the signal delay (the Shapiro effect), and path-bending of the radiosignal propagation in the gravitation field of the Sun, Jupiter, Saturn and the reduction of observations from the proper time of the observer to the coordinate time of the ephemerides are taken into account while processing observations.​

    Fienga A. et al., "INPOP08, a 4-D planetary ephemeris: From asteroid and time-scale computations to ESA Mars Express and Venus Express contributions," Astronomy & Astrophysics 507:3 (2009)
    http://www.mendeley.com/research/in...mars-express-and-venus-express-contributions/
    With INPOP08, we aim to produce planetary ephemerides as fully compatible as possible with the relativistic background recently adopted by the astronomical community and summarized by the IAU2000 and IAU2006 conventions (Soffel el al., 2003).​

    I'd provide one on the DE series from JPL as well, but unfortunately, JPL appears to be suffering a massive connection failure right now.


    That is a trivial problem. Try using GR as-is (no post-Newtonian expansion) for a solar system comprising a central star, 8 planets (one of which is rather large), a growing bunch of dwarf planets and minor planets, dozens of sizable moons, hundreds of sizable asteroids, etc. It is utterly intractable.
     
  18. Nov 20, 2011 #17
    Yes you are correct!
    I did not know how advanced the calculations already are.
     
    Last edited: Nov 20, 2011
  19. Nov 20, 2011 #18
    Actually, I am using the precession of Mercury reported by Tai L. Chow in his 2008 book "Gravity, black holes, and the very early universe". Whatever frame he used. This differs from Clements value by almost an arcsecond per century. I did not see a reference in the summary of the book available online. It may be that Chow used R.L.Duncombe.

    The secondary question, then, reduces do where can I find the observed precession of Mercury relative to the ICRF?

    Observed orbital parameters for Mercury to the thousandths of a degree from 1970 to 2010 would more than suffice.
     
  20. Nov 20, 2011 #19

    D H

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    The number in Chow, 43.11±0.45″ is the exact same number, including the uncertainty, as my 1970 version of Marion which references Duncombe.

    Sigh. You don't. The perihelion precession of Mercury is a solved problem. Physicists are not paid to re-solve problems that were solved a century ago. They are paid to solve today's problems.
     
  21. Nov 20, 2011 #20
    As D.H. writes the matter is lock, stock and barreled, all influences up to moons are taken into account including lower order relativistic effects (higher order is really irrelevant as all this is weak field GR) and it all matches perfectly so it is a done deal.
    End of story, the theory and experiment are the same.
     
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