Galactic torsion fields


1 Summary


Following the detection of spin torsion radiation from the Sun there arose a question as to whether spin torsion radiation was radiated from other sources.

This question was investigated by a method that relied on screening an interferometer from different directions and checking to see if the screening had any effect. Other smaller devices that also responded to spin torsion radiation were also used to try to improve the accuracy. These early experiments gave positive results and indicated that there was at least one other source of radiation and that source was approximately in the direction in which the Solar System was travelling through the galaxy.

The experiment described here used the same equipment that was used to investigate spin torsion radiation from the Sun. The accuracy of the equipment allowed a source of spin torsion radiation to be identified that appeared to come from galactic longitude 90° latitude 0°.

The radiation coming from galactic longitude 90° latitude 0° was passed between the poles of a powerful permanent magnet before it reached the measuring apparatus. It was found that the radiation beam was deflected by 0.75 degrees to the left or right depending on the polarity of the magnetic field. This result was identical to the result from applying a magnetic field to spin torsion radiation from the Sun.

There is a problem in making any assumptions about the results. When the apparatus used in this experiment was used to investigate spin torsion radiation from the Sun it was found to be responsive to radiation from the Sun's true rather than the optical position. Because of this it is not possible to be sure that the radiation detected in this experiment does not actually come from the true position of some galactic object.


2. Introduction

First attempts at locating another field were made using a so called Dual Mass Device (DMD) developed by A.N.Coll for other purposes and supplied by him. A DMD uses two small cylindrical masses - typically 1 cm diameter and 1cm deep, spaced apart on a brass rod by 10cm. The rod is supported using a brass stand. The device creates an interference fringe whose distance can be adjusted by changing the spacing between the masses.

To search for another field one of the masses was screened in various different directions by crossed Spin Polarisers. For each direction of the screen checks were made to see if any changes occured to the fringe distance. This work established that there was another field and with the help of C. M. Humphries it was narrowed down to the Cygnus constellation. This is the direction that the Solar System is travelling through the galaxy.

In order to determine the origin of what we now call the Galactic field with more accuracy the pivoting tube system that was used to investigate the torsion field from the Sun was used. The position of the Sun at a particular time provided a reference angle to help align the apparatus.


3. Equipment

Figure 1 shows a 1 metre long Aluminium tube a which passes through wooden block e which can be pivoted up and down (in altitude). The pivot angle is measured using a digital inclinometer.

Baseboard f can itself be pivoted horizontally about b (in azimuth) with respect to g. The baseboard is 1 metre long and has an angle scale h at the opposite end to pivot b. All of the pivots are of brass.

Once the initial direction of the baseboard has been set, the whole assembly can be adjusted by plus or minus five degrees from the nominal angle using scale h which is marked in 0.1° intervals.

Pivot block e has a white painted face c. In use the azimuth angle of the equipment can be determined by aligning it with the Sun by minimising the shadow of the tube on face c.

Figure 2 is a partial top view showing the direction r of the incoming spin torsion radiation from the north. The pole pieces of a large permanent magnet m are shown in the top view. These pole pieces are only in place when investigating the effect of magnetic fields on the incoming radiation.


Fig. 1  Pivoting tube


Fig.2  Pivoting tube top view



4. Measurement of spin torsion fields from the galaxy

The first part of the measurement process was to find a time at which the location of galactic longitude 90° latitude 0° moved horizontally across the sky. Using Cybersky software it can be seen that this occurs when tube a is pointed in the 0° direction. In this direction the change in altitude over the twelve minutes for which measurements were made was less than 1 minute of arc. This allowed the altitude of tube a to be set to a fixed value that was correct for the duration of the experiment.

The azimuth of the tube had to be accurately set to 0°. To do this the left hand end of the tube in figure 1 was aligned with markings on the floor of the experimental area so that it was pointed in a southerly direction. On a sunny day the time at which the shadow of the sun on face c in figure 1 disappeared was noted. (adjustment of the altitude of the tube was allowed in order to do this but the azimuth remained unchanged). Using Cybersky software the azimuth angle of the Sun at the noted time was found, this gave the angle of the floor markings.

Because the galactic longitude 90° latitude 0° point was in the northern sky, the left hand end of tube a was used to point at it. The azimuth angle of the tube was adjusted from the angle of the floor marking to the zero° (north/south) position using a digital protractor. The elevation of the tube was set to the expected elevation using a digital inclinometer.

A measuring tape was laid on the floor from tube a to the west at right angles to the apparatus. Using copper detector rods measurements of the fringe distance to the nearest 100mm were made at one minute intervals before and after the time at which the galactic longitude 90° latitude 0° point transited across the tube pointing position.


Figure 2.  


The tube was set to azimuth 0 and altitude 14.5 degrees for a transit of galactic 90° 0° at 20:51 UTC on the 31st March 2022 in Edinburgh. Figure 2 shows that there was a response at 20:52



5. Deflection of spin torsion radiation by magnetic fields.

The magnetic pole pieces m shown in figure 2 were put in place. The field strength across the pole pieces was 6000 µT. It was found that as in the experiment on spin torsion fields created by the Sun, the radiation beam was deflected and could only be restored by re-aligning tube a 0.75° degrees to the left or right. For the full results of this effect when tube a was pointed at the Sun the reader is directed to the results in the experiment.


6. Discussion

Figure 2 shows that the fringe pattern created by the tube occurred one minute later than the calculated time of 20:51 UTC. Because the apparent movement of the galactic 90° 0° point across the sky is caused by the Earth's rotation, the 1 minute difference corresponds to an angular error of 0.25°.

It does appear that spin torsion radiation is coming from the direction that the Solar System is travelling through the Galaxy, however some caution is needed in coming to this conclusion. The radiation from the Sun experiment found that radiation from the Sun came from its real position rather than its optical position. It is possible that the radiation identified in this experiment also comes from the real position of some galactic object. The difficulty is that even though we know the optical position of galactic objects we have no idea of their real position because we don't know how long spin torsion radiation from them takes to reach us.

Work carried out by M. M .Lavrentiev, V. A. Gusev, I. A .Eganova, M .K. Lutset and S. F. Fominykh [1] using the 2m telescope at the Crimea national observatory used a special resistor at the focal point of the telescope which was blanked off to visible light. This equipment had been used to investigate the true position of the Sun. It was claimed that the equipment could measure the angular distance between the optical position of a Star and its true position.

7 References

[1] M. M.Lavrentiev, I. A .Eganova, M .K. Lutset and S. F. Fominykh
Remote effect of stars on a resistor. Dokl. Akad. Nauk SSSR 314, 352-355 September 1990
Translated in Sov. Phys. Dokl. 35(9), September 1990 pp 818-82.



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