Radio Astronomy and Cosmology
Seiten
2002
|
1977 ed.
Kluwer Academic Publishers (Verlag)
978-90-277-0838-0 (ISBN)
Kluwer Academic Publishers (Verlag)
978-90-277-0838-0 (ISBN)
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Proceedings of IAU Symposium No. 74, held in Cambridge, England, 16-20 August 1976
337 F(e) = (z) where the angle between the directions III and 112 is equal to 8. r is the angular diameter effective distance of the epoch for recombination. F (8) ve have F(e): f (e) (S" ) e. . is a Bessel function. It is assumed here that the spectrum of gravitational waves takes the form 1/ hI'::: hoK for all relevant wavelengths, a is beam width of the radio antenna, d/= d, and is the duration of the process of recombinations in /-time. The results for different beam widths are shown in Fig. 1. 338 I. D. NOVIKOV 1-. . . -__ 0. 5 1 1. 5 2 e' 0. 5 o and for a l' (solid line) and Fig. 1. The function f(8) for n for a = 2' (dotted line). These formula should be used in analysing the implications of future observations. Comparison with the observational data now available enables us to establish an upper limit for the energy density of long gravitational waves. This method is most sensitive for gravitational waves with A ct The fluctuations; due to these waves have scale 0. 03 GW rec 4 radian. If, according to modern observations, we take;
337 F(e) = (z) where the angle between the directions III and 112 is equal to 8. r is the angular diameter effective distance of the epoch for recombination. F (8) ve have F(e): f (e) (S" ) e. . is a Bessel function. It is assumed here that the spectrum of gravitational waves takes the form 1/ hI'::: hoK for all relevant wavelengths, a is beam width of the radio antenna, d/= d, and is the duration of the process of recombinations in /-time. The results for different beam widths are shown in Fig. 1. 338 I. D. NOVIKOV 1-. . . -__ 0. 5 1 1. 5 2 e' 0. 5 o and for a l' (solid line) and Fig. 1. The function f(8) for n for a = 2' (dotted line). These formula should be used in analysing the implications of future observations. Comparison with the observational data now available enables us to establish an upper limit for the energy density of long gravitational waves. This method is most sensitive for gravitational waves with A ct The fluctuations; due to these waves have scale 0. 03 GW rec 4 radian. If, according to modern observations, we take;
| Erscheint lt. Verlag | 1.4.2002 |
|---|---|
| Reihe/Serie | International Astronomical Union Symposia (Closed) ; v. 74 |
| Zusatzinfo | 6 black & white illustrations, biography |
| Verlagsort | Dordrecht |
| Sprache | englisch |
| Maße | 156 x 234 mm |
| Gewicht | 765 g |
| Einbandart | gebunden |
| Themenwelt | Naturwissenschaften ► Physik / Astronomie ► Astronomie / Astrophysik |
| Naturwissenschaften ► Physik / Astronomie ► Theoretische Physik | |
| ISBN-10 | 90-277-0838-X / 902770838X |
| ISBN-13 | 978-90-277-0838-0 / 9789027708380 |
| Zustand | Neuware |
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