: : : : : : :
: : : : Дорогой Дмитрий Павлов!
: : : : Все-таки, чем отличается финслерова геометрия от геометрии Декарата, геометрии нашей Вселенной?
: : : : И для чего Вам нужна другая геометрия, которая отличается от реальной геометрии землевладельцев (имеется в виду люди, владеющей планетой Земля)?
: : :
: : : К сожалению у меня не получается объяснить это даже людям разделяющим концепции СТО, ОТО и КМ. С Вами у меня вообще нет ни единого шанса. Не обижайтесь..
: :
: : Как известно, "если физик/математик не способен объяснить своей уборщице суть теории, то он не знает этого сам".
: : Эти слова приписываются многим ученым: Ферми, Эйнштейну, Резерфорду, Мигдалу и проч.
: :
:
: : Вот самый главный вопрос: какой транспортный процесс (переносящий информацию) является в Вашей теории эталонным, - детектирующим кривизну пространства? - Очевидно, что свет. Но ведь ЭМ-сигнлаы лишь "одни из...". Тогда Вы описываете всего лишь какую-то частную визуально наблюдаемую модель Мира. А в Мире на больших масштабах ЭМ-поля не шибко влияют на движение объектов. На движение световых сигналов - да, влияют. Но тогда Вы описываете оптические иллюзии (явления) и то частные, а не сущность. А можно ли в таком случае так надеяться на всеобщность Ваших рассуждений о "геометрии мира"?
:
: Как Вы представляете себе точность дальнометрических измерений в лазерной дальнометрии Луны и радиолокационных измерений расстояний до планет и космических зондов?
:
: http://quasar.ipa.nw.ru/PAGE/DEPFUND/LEA/RUS/ruslea.htm
:
: http://vivovoco.rsl.ru/VV/JOURNAL/NATURE/09_02/090...
http://iau-comm4.jpl.nasa.gov/GAK.pdf
http://iau-comm4.jpl.nasa.gov/EPM2004.pdf
Здесь далее выдержка из EPM2004.pdf:
"RADAR AND OPTICAL OBSERVATIONS
AND THEIR PROCESSING
The EPM2004 ephemerides were fitted to 317041 position
observations (1913-2003) of various types, including
radiometric measurements of planets and spacecraft,
CCD astrometric observations of outer planets
and their satellites, and meridian and photographic
observations. The data used for the production of the
EPM ephemerides were taken from the JPL database
(http:/ssd.jpl.nasa.gov/iau-comm4/), developed and
maintained by Dr. Standish, and from the database of
optical observations of Dr. Sveshnikov, and were
extended to include Russian ranging observations of
planets made in 1961-1995 (available from the site of
the Institute of Applied Astronomy of the Russian
Academy of Sciences, //www.ipa.nw.ru/PAGE/DEPFUND/
LEA/ENG/englea.htm). All observations used to
construct the ephemerides are described in Tables 2 and 3.
Ranging observations of planets started in 1961 and
have become widely used in astronomical practice
since then, making it possible to determine various
astronomical constants with high precision. Reductions
of radar observations including relativistic corrections-
the delay of the radio signal near the Sun (the
Shapiro effect); the transition from the coordinate time,
the argument of ephemerides, to the proper time of the
observer; the delay of radio signals in the Earth's troposphere and in the plasma of the solar corona-are well
known, and a description of them can be found, e.g., in
the paper by Standish (1990). Only the reduction for the
topography of the planets may cause some problems.
Topographic correction of observations of Mars and
Venus was performed using modern hypsometric maps
of the surfaces of these planets and a representation of
the global topography with an expansion of spherical
functions of 16th-18th degrees. The global topography
of Mercury is unknown, and, therefore, we represented
it by the second-order Legendre functions. The coefficients
of the harmonics were estimated from ranging
observations of Mercury (Pitjeva, 2001b).
We should point out the special importance of ranging
observations of the Martian landers Viking 1 and 2 (1976-1982), which are free of topographic errors, errors that persist in ranging observations of planets despite careful topographic reductions. These observations remained the most accurate position observations of planets for 20 years (they have an a priori accuracy of about 10 m). The data from the new Pathfinder lander were received during three months in 1997. The computation of the positions of the landers on the surface of Mars in the ephemeris reference frame requires a theory of Martian rotation that includes not only precession and nutation of the rotation axis of Mars but also seasonal terms in the Martian rotation (see Youder and Standish, 1997; Folkner et al.
, 1997; Pitjeva, 1999).
Since 1998, the database has been augmented by ranging observations of the Mars Global Surveyor (MGS) spacecraft, and, since 2002, by the Odyssey spacecraft.
These measurements have an accuracy of 2 m.
All observations of Mars and, as a rule, those of
Mercury and Venus, performed during one day and,
after introducing all the required corrections, including
the reduction for the topography of the planets, were
grouped into normal places. The normal places for the MGS and Odyssey data were obtained by combining
the measurements made during the same session: it was
assumed that the measurements belong to different sessions
if the corresponding observation times differed by
more than one hour. When combining observations, we
assigned weight to all observations according to their a
priori accuracy, which is usually given in the corresponding publications.
Unfortunately, unlike the observations of the
Viking spacecraft, which were made at two frequencies and,
therefore, allowed the delay in the solar corona to be
taken into account, the MGS and Odyssey observations
were carried out at one X band and the effect of the solar
corona delay was considerable, especially near the
superior solar conjunctions in 1998 and 2002. We
reduced these observations using the following model
of the solar corona:
см. формулу в источнике PDFe
is the electron density. We determined the parameters B and from observations, and these parameters differed for different conjunctions.
Although this reduction for the effect of the solar corona substantially reduced the residuals of the observations,
the remaining influence of the corona is still obvious (Fig. 1 for MGS and Odyssey). Moreover, the parameters of the corona correlate with other parameters and impair their determination. This fact must be taken into account in high-precision astrometric observations in future space missions.
For Jupiter, unlike other outer planets, a number of
precise radiotechnical observations by spacecraft
(Pioneer 10 and 11, Voyager 1 and 2, Ulysses, and
Galileo) approaching the planet or orbiting it have
been performed, which allow its orbit to be determined
much more accurately than those of other outer
planets.
Figure 1 shows the residuals of ranging observations.
The root-mean-square errors of fits to observations
are equal to 1.4 km for Mercury; 0.7 km for Venus
and Mars; 8 and 4.4 m for the Viking and Pathfinder
landers, respectively; and 1.4 m for MGS and Odyssey."
отредактировано 30.01.2007 16:37 |
» Альтернативный форум