Point #1-The Universe Accelerating
Science Discovery of the Year: 1998
By 1995, most scientists had accepted the "Big Bang" theory based on theory and observation. The idea that the universe is getting bigger (expanding) was as certain as you are reading these words. And just as certain was the idea that after the initial Big Bang event, gravity would be slowing the rate of expansion. However, the world of scientific thought received a rude awakening.
After 10 years of intense research and observing distant supernova, two independent scientific teams (the Supernova Cosmology Project and the High Z Supernova Search Team Project) came to the same conclusion that the rate at which the universe is expanding is accelerating (getting bigger at a faster and ever faster rate). This idea was totally unexpected and is typically called the Accelerating Universe.
Point #2- Overall Mass is decreasing Gravitational wave dectors
Currently there are 5 such instruments in operation around the world. The are working in cooperation, with least two detectors in continuous coincident operation since 1993. The experiments are ALLEGRO, AURIGA, EXPLORER, NAUTILUS, and NIOBI. Some of the groups associated with these instruments are planning new experiments to make detectors of much greater sensitivity.
ALLEGRO ALLEGRO is an experiment operated by the Louisiana State University in Baton Rouge, Louisiana, USA. This experiment employs an aluminum bar cooled to 6°K. It operates at a frequency of 900 Hz, and has a strain sensitivity of 7×10-19 Hz-1/2. ALLEGRO has had two data runs, with the first covering June 1991 through January 1995, and the second covering 1996 to the present time. The experiment was operating when supernova 1993J occurred; no gravitational waves were detected.
AURIGA
The
AURIGA detector is run by the Instituto Nazionale di Fisica Nucleare (INFN) in Legnaro, Italy. It is an aluminum bar cooled to 0.1°K. It operates at a frequency of 900 Hz, with a sensitivity of 3×10-19 over its first data run. AURIGA has been upgraded and between January 13th and May of 2004 it has been undergoing calibration and diagnostics. The sensitivity of the instrument has been improved.
EXPLORER
The
EXPLORER detector is based at CERN and operated by the University of Rome. It is a 2270kg aluminum bar cooled to 2° K. It operates at the resonance frequencies of 906 and 923 Hz, and has a strain sensitivity of 7×10-19.
NAUTILUS
The
NAUTILUS detector is run by the Instituto Nazionale di Fisica Nucleare (INFN) at the Laboratori Nazionali di Frascati Italy. It is a 2300kg aluminum bar cooled to 0.1°K. It operates at the resonance frequencies of 908 and 924 Hz. NAUTILUS has a sensitivity of 6×10-19.
NIOBE
The university of Western Australia operates the
NIOBE detector at Perth, Australia. It is a niobium bar operating at a temperature of 5°K. It is sensitive at the frequency of 700 Hz and has a sensitivity of 5×10-19.
1 Ju, L., Blair, D.G., and Zhau, C.
“Detection of Gravitational Waves.” Reports on Progress in Physics 63 (2000): 1317–1427.
Some evidence to role in- Later Broadband Gravitational-Wave Pulses from Binary Neutron Stars in Eccentric Orbits A. V. Gusev,1
V. B. Ignatiev,2
A. G. Kuranov,1
K. A. Postnov,1,3 and
M. E. Prokhorov1
1Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119899 Russia
2Moscow State University, Vorob'evy gory, Moscow, 119899 Russia
3Max-Planck-Institut für Astrophysik, Karl Schwarzschild Strasse 1, 86740 Garching bei München, Germany
(Received October 25, 2001) The gravitational-wave radiation from binary stars in elliptical orbits peaks at times close to the periastron passage. For a stationary distribution of binary neutron stars in the Galaxy, there are several systems with large orbital eccentricities and periods in the range from several tens of minutes to several days from which gravitational-wave radiation at periastron will be observed as a broad pulse in the frequency range 1–100 mHz. The LISA space interferometer will be able to record pulsed signals from these systems at a signal-to-noise ratio S/N > 5
in the frequency range ~10–3–10–1 Hz. Algorithms for detecting such signals are discussed.
©2002 MAIK "Nauka / Interperiodica". More GRAVITATIONAL WAVES FROM BINARY
NEUTRON STARS
D. Gondek-Rosinska
(1), M. Bejger (1), E. Gourgoulhon(2), K. Taniguchi(2), T.
Bulik (1), L. Zdunik(1), P. Haensel(1)
(1) CAMK, PAN, Bartycka 18, 00-716 Warsaw, Poland
Coalescing neutron star binaries are expected to be among the
strongest sources of gravitational radiation to be seen by laser
interferometers. I will present the results of our studies of
relativistic quasiequilibrium sequences of close binary systems
composed of neutron stars described by realistic equations of state.
I will focus on characteristic features in the waveform that will help
to distinguish between different models of dense nuclear matter. The
calculation are done for different mass ratios of neutron stars taking
into account both the properties of the known double neutron star
binaries and recent results obtained by using the well tested
StarTrack binary population synthesis code (Bulik, Gondek-Rosinska,
Belczynski 2003).
There is much more indirect evidence to date but my point, without getting too specific is this-
The force of the Universe is constant The matter in the universe is changing form from a broad defination of mass (three D matter) to the gravitational wave. Space is enlarging as mass is shrinking or bound matter is decaying as unbound matter is generated.
Now here is a jump- If absolute time is defined as the observation of this process, or an action of this decay process then this process answers how time is changable do to motion due to gravitational wave preceptions relative to point of origin. you know the way sound is changable do to motion.
If you have a better explaination, lets here it?