Regensburg 1998 – wissenschaftliches Programm
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GR: Gravitation und Relativitätstheorie
GR 4: Gravitationswellen, Lichtausbreitung im Gravitationsfeld
GR 4.1: Hauptvortrag
Donnerstag, 26. März 1998, 09:30–10:15, H47
Gravitational Wave Astronomy in terms of Large Radio Telescopes — •Sergei M. Kopeikin — FSU Jena, TPI, Max-Wien-Platz 1, D-07743, Jena, Germany
Search for gravitational waves (GW) is one of the most important directions in developments of modern relativistic astronomy. The spectrum of GW extends through the entire frequency range from extremely low frequencies f ∼ 10−18 Hz to the high frequency band f ∼ 1 ÷ 104 Hz. Ground- and space-based laser GW detectors will be sensitive to frequencies from 1 Hz to 1 kHz. On the other hand, timing of single and binary pulsars [1] as well as VLBI radio observations of quasars [2] open the good opportunity for detection of low frequency waves among which pulses of long GW from colliding supermassive black holes and/or AGNs and stochastic background of gravitational radiation (GWB) in the early universe are to be essentially interesting. We describe the main sources of low frequency GWs in more detail along with the theoretical foundations of gravitational wave astronomy on the basis of large radio telescopes. In particular, sources and statistical properties of colored noises corrupting the GW signal are discussed as well as a brief introduction given to data analysis techniques. In conclusion, existing limits on energy density Ωg of GWB and their future possible improvements are outlined.
[1] Kopeikin S. M., Phys. Rev. D, 56, 4455 (1997)
[2] Gwinn, C. R., Eubanks, T. M., Pyne, T., Birkinshaw, M., Matsakis, D. M., Astrophys. J., 485, 87 (1997)