log spiral stretching

log spiral stretching

By Henryk Szubinski


basically what makes the universe a bit larges as from 3 x rotations of a log spiral to a 6 x increase where the boosted values of photons is + 1/2 of a c vector as well as the 0.5 increase of the universe:

by defining the universe as = 1

and the photon = 1

the values of x 3 and x 6 = sum of x 18 meaning that a common value 0.5 will define the mean by ; 18 +.5+.5 = 19 /3

or the universes new value that will define no photon limitations or any universe limits as 6.3 LOG TAN



File:Messier51 sRGB.jpg

In polar coordinates (r,θ) the curve can be written as[1]

r = ae^{b\theta}\,


\theta = \frac{1}{b} \ln(r/a),

with e being the base of natural logarithms, and a and b being arbitrary positive real constants.

In parametric form, the curve is

x(t) = r \cos(t) = ae^{bt} \cos(t)\,
y(t) = r \sin(t) = ae^{bt} \sin(t)\,

with real numbers a and b.


The arms of spiral galaxies often have the shape of a logarithmic spiral, here the Whirlpool Galaxy

logarithmic spiralequiangular spiral or growth spiral is a special kind of spiral curve which often appears in nature. The logarithmic spiral was first described by Descartes and later extensively investigated by Jacob Bernoulli, who called it Spira mirabilis, “the marvelous spiral”.

.basics of using a log tan spiral to stretch out its spiral format into a string by what is defined as UNWINDING

will in general cases of relation to a star such as a white dwarf =the action of pulling out or stretching the spiral log tan values by

S = displacement of the pull

S root = the resultant length difference of the string as the values of 1/2 c or photon waveform value

as well as the total of a log tan spiral in its full value = 3 rotations by a exponential increase of the shortening of a exit size outof the universe will be shown to have higher levels of universal exit size by the stretching as 2 x larger meaning that the universe can have a x 6 or x 7 to x 10 size increase of absolute measurements..

4  x STRING S=0.5c Universe



Image of Sirius A and Sirius B taken by the Hubble Space Telescope. Sirius B, which is a white dwarf, can be seen as a faint pinprick of light to the lower left of the much brighter Sirius A.

File:Sirius A and B Hubble photo.jpg

A white dwarf, also called a degenerate dwarf, is a small star composed mostly of electron-degenerate matter. They are very dense; a white dwarf’s mass is comparable to that of the Sun and its volume is comparable to that of the Earth. Its faint luminosity comes from the emission of stored thermal energy.[1] In January 2009, Research Consortium on Nearby Stars project counted eight white dwarfs among the hundred nearest star systems of the sun.[2]The unusual faintness of white dwarfs was first recognized in 1910 by Henry Norris Russell, Edward Charles Pickering, and Williamina Fleming;[3], p. 1 the name white dwarf was coined by Willem Luyten in 1922.[4]


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