Doppler Shift

The Doppler Shift of light is the change in frequency of a wave in relation to an observer who is moving relative to the wave source. It was named after the Austrian physicist Christian Doppler, who described the phenomenon in 1842. Light waves from a moving source experience the Doppler shift as either a redshift or blueshift in the light's frequency. When an object approaches the observer its light will blueshift, and when it recedes from the observer its light will redshift.

Discussions on this topic typically ask how the galaxies can be redshifted if they are not receding away from the observer at very high velocities, as is suggested by the traditional expanding universe model which postulates that space is expanding in every direction. An answer to this query is that since in FE it is acknowledged that the Sun is a different entity than a galaxy, the properties of those entities, or the properties of the mediums the light must pass through to reach the observer, may be entirely different.

Indeed, the Doppler Shift of light is only one interpretation for the redshifts. In Highlights of Astronomy, Vol 9, the International Astronomical Union explains:

Jacques Moret-Bailly
Physics Professor Jacques Moret-Bailly of the University of Burgundy has written a number of papers on physical alternatives to Doppler Shift.

Correspondence of classical and quantum irreversibilities

Abstract

Conclusion

The coherent Raman scattering in astrophysics; application to a new model of quasar (Archive)

Propagation of Light in Low-Pressure Ionized and Atomic Hydrogen: Application to Astrophysics

Abstract

Sol Aisenberg
From the chapter Redshift errors of How To Understand The True Cosmos by Applied Physicist Sol Aisenberg (bio) we read:

Alternative Redshift Theories
The website plasma-universe.com lists a number of alternative redshift theories at https://www.plasma-universe.com/redshift/ (Archive)

Censorship
Redshift researchers complain of censorship in science:

Noncosmological Redshifts Geoffrey Burbridge Astronomical Society of the Pacific

https://www.jstor.org/stable/10.1086/322152

Introduction

Conclusion