Abstract

To date, astronomical observations and studies have failed to detect solar gravitational waves. By developing a new, promising detection method, the author of this paper has succeeded in detecting gravitational waves emitted by the Sun. This detection method relies on ultrasonic technology, which is new and original, and enables reliable gravitational wave detection. The technology underlying the method relies on the creation of two independent measuring channels with acoustically transparent media, in which ultrasonic waves prop agate in opposite directions. To ensure the method's operation in acoustically transparent media, specific nonlinear conditions for ultrasonic wave propagation are created. This transforms the ultrasonic waves into test bodies suspended continuously in the acoustically transparent media. These test bodies, in the form of ultrasonic waves, are directly exposed to gravitational waves as they propagate through nonlinear media. By differentially separating mutual alternating phase shifts and fluctuations of ultrasonic waves traveling in op posite directions through two channels of acoustically transparent nonlinear media, gravitational waves are reliably detected directly. This results in a direct effect of gravitational waves on test bodies, which represent ultrasonic waves. The physical essence of this direct effect lies in the fact that gravitational waves represent alternating accelerations propagating through space at high speed. These accelerations cause alternating ac celerations of counter-propagating ultrasonic waves, which are mutually detected. This is the simplicity and fundamental nature of the detection method. The ultrasonic detector created in this way allows for continuous observation of numerous gravitational waves from our Sun. Gravitational waves and signals from numerous stars in our Galaxy, including the Universe as a whole, are also observed. Observations of solar gravitational waves have yielded evidence of their enormous propagation speed compared to the speed of light. In particu lar, it has been found that the propagation speed of gravitational waves is at least three orders of magnitude greater than the speed of optical waves. The detector allows selective listening to solar gravitational waves in the audio frequency range. Evidence has been obtained that, in most observations, the signal level of solar gravitational waves caused by coronal mass ejections or local solar flares is comparable to the signal level of gravitational waves caused by both supernova explosions and possible black hole mergers.* Therefore, observing solar gravitational waves can and should be a test of the sensitivity and efficiency of gravitational observatories being developed and operating. This circumstance is important for confirming the objectivity and validity of the obtained results. Objectivity will prevail if the expensive gravitational observatories cur rently in operation obtain tangible evidence of the detection of gravitational waves caused by coronal mass ejections and flares from our nearest star, the Sun.

DOI: doi.org/10.63721/25JPQN0135

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