**6. Conclusion**

*<sup>f</sup>* <sup>¼</sup> <sup>1</sup>*:*<sup>71</sup> � <sup>10</sup>�<sup>7</sup> *<sup>T</sup>* <sup>∗</sup>

of elementary particles *g* <sup>∗</sup> ¼ 106*:*75).

of relic gravitational waves.

*Progress in Relativity*

required level.

depend [4, 23, 24].

**230**

LISA project is scheduled for 2029.

*GeV g* <sup>∗</sup>

where *g* <sup>∗</sup> is the effective number of the degrees of freedom (in standard model

Therefore, conditions (18) and (21)–(23) impose restrictions on the parameters

The application to the analysis of the models of the early universe only of the slow-roll approximation implies a low-frequency spectrum of relic gravitational waves in the range of 10�<sup>18</sup> � <sup>10</sup>�<sup>16</sup> Hz [20]. However, the predominance of the kinetic energy of the scalar field during the evolution of the early universe provides a theoretical justification for the existence of high-frequency relic gravitational waves in models with one scalar field in the range of 10<sup>2</sup> � <sup>10</sup><sup>4</sup> Hz [21] which can be used as affordable means of verification of models of the early universe in the presence of physical effects that increase the sensitivity of the detector to the

Currently, the most productive method of direct detection of gravitational waves is the use of interferometers as detectors, which was proposed in the article by Gertsenshtein and Pustovoit [22]. This principle is widely used in modern laser interference gravitational antennas, the main element of which is the Fabry-Perot interferometer. These are broadband gravitational antennas,

After creating the first laser interferometer for detecting gravitational waves, systematic work began on the creation and improvement of such devices in various laboratories around the world. The experience of gravitational antenna projects by VIRGO (Italy, France), LIGO (USA), TAMA (Japan), CLIO (Japan), GEO-600 (Germany), and OGRAN (Russia) will certainly be used to create more compact and highly sensitive antennas of new generation [4]. Also, as the most promising project for the direct detection of gravitational waves, work on the creation of a space interferometer in a helio-stationary orbit should be noted, in which the distance between the mirrors will be about 1 million kilometers. This project is called Laser Interferometer Space Antenna (LISA) [25]. The implementation of the

One of the promising methods for increasing the sensitivity of gravitational antennas in the high-frequency region of the spectrum is to use the phenomenon of low-frequency optical resonance, which distinguishes this approach from other projects on the detection of gravitational waves. The presence of this effect in Fabry-Perot interferometers was first considered in [23, 24]. At the moment, there is a high-frequency gravitational wave detector, which was built at the University

of Birmingham, United Kingdom [26]. Also, it is planned to build the

Thus, at the moment there are a large number of promising methods for direct observation of gravitational waves, which correspond to the ability to measure the characteristics of relic gravitational waves for a better understanding

high-frequency gravitational wave detectors in Japan [27].

of the physical processes occurring in the early universe.

which offer a lot of opportunities as to the methods of recording of gravitational waves and extracting signals, as well as the use of quantum non-perturbative measurements and the inclusion of gravitational antennas in the network. The main element of laser interference gravitational antennas, as a rule, is Fabry-Perot multipath free-mass resonator, on whose properties the sensitivity and noise immunity of the entire gravitational antenna largely

106*:*75 �1*=*<sup>6</sup>

*Hz* (31)

We considered the basis of building and verifying of the inflationary models of early universe. As the method for constructing the exact cosmological solutions corresponding to observational constraints, the models with generalized exponential power-law dynamics are proposed.

The verification of the relevance of such models is related to the estimation of the contribution of relic gravitational waves to the anisotropy and polarization of the cosmic microwave background radiation. Therefore, there are a lot of inflationary models with different scalar field potentials that will satisfy the observational constraints.

The most obvious way to significantly reduce the number of theoretical models of cosmological inflation is direct detection of relic gravitational waves.

The most promising methods in this area of experimental research are using the interferometers as detectors. The interesting direction of the observation is the detection of high-frequency relic gravitational waves using the effect of low-frequency optical resonance proposed in [23, 24].
