P. Amico

Low-frequency internal friction in silica glass

Precise low-frequency internal friction measurements on vitreous silica, taken over a wide temperature (4 K 160 K the loss angle develops a distinct step-like structure followed by a plateau, both independent of ν, thus signalling the onset of a competing relaxation mechanism with much higher an activation energy. Copyright c EPLA, 2007

Cosmic-ray spectra near the LISA orbit

Cosmic-ray particles traverse the LISA apparatus charging the proof masses. This process causes spurious Coulomb forces between the test masses and the surrounding conducting surfaces mimicking gravitational wave signals. Approximately 13 g cm−2 of matter overlies the proof masses. The nucleonic component of cosmic rays (about 99% of the total) below 100 MeV/n stops inside the spacecraft without reaching the masses. It is of major importance to determine the primary and solar cosmic-ray particle fluxes above this energy near the LISA orbit in order to predict the effect on the apparatus.

A parallel Beowulf-based system for the detection of gravitational waves in interferometric detectors

The detection, in a modern interferometric detector like Virgo, of a gravitational wave signal from a coalescing binary stellar system is an intensive computational task both for the on-line and off-line computer systems. A parallel computing scheme using the Message Passing Interface (MPI) is described. Performance results on a small scale cluster are reported.

Fused silica suspension for the VIRGO optics: status and perspectives

Thermal noise in mirror suspension wires is the main limitation of low-frequency sensitivity of interferometric gravitational wave detectors. In order to minimize the pendulum thermal noise, a monolithic design, using a low dissipation material, is proposed for VIRGO. High mechanical Qs and high breaking strengths have been obtained for monolithic fused silica fibres. A low-dissipation and high-strength bonding technique using potassium silicate bonding is proposed.

LISA test-mass charging process due to cosmic-ray nuclei and electrons

Solar energetic particles and galactic cosmic rays with energies larger than 100 MeV cause progressive charging of the LISA experiment test masses. Consequently, Coulomb forces occur between the test masses and the surrounding conducting surfaces generating spurious signals that might be mistaken for gravitational wave signals. We have parametrized the energy spectra of galactic cosmic-ray nuclei and electrons near the LISA orbit in order to evaluate their role in the test-mass charging relative to the most abundant proton component. This work has been carried out using the FLUKA Monte Carlo program.

Simulation of the charging process of the LISA test masses due to solar particles

Cosmic-ray and solar particles above 100 MeV penetrate the LISA experiment test masses. Consequently, electric charges accumulating there generate spurious Coulomb forces between the masses and the surrounding electrodes. This process increments the noise level of the experiment. We have estimated the amount of charge deposited per second on the LISA test masses by primary cosmic-ray protons at solar minimum and solar maximum and by solar energetic particle (SEP) events. This simulation has been carried out with the Fluka Monte Carlo program. A simplified geometry for the experiment has been considered. We have found an effective charge rate of 110 e s−1 for primary protons at solar maximum and 150 e s−1 at solar minimum between 0.1 and 1000 GeV. The amount of charge released by a medium intensity gradual event (7 May 1978) varies from 206 e s−1 in the first few minutes to 4575 e s−1 at the peak of the event. At the occurrence of medium or strong solar events, the LISA sensitivity curve at frequencies lower than 3 × 10−4 Hz is dominated by the noise due to the test-mass charging process.

Monocrystalline fibres for low thermal noise suspension in advanced gravitational wave detectors

Thermal noise in mirror suspension will be the most severe fundamental limit to the low-frequency sensitivity of future interferometric gravitational wave detectors. We propose a new type of materials to realize low thermal noise suspension in such detectors. Monocrystalline suspension fibres are good candidates both for cryogenic and for ambient temperature interferometers. Material characteristics and a production facility are described in this paper.

Mechanical quality factor of mirror substrates for VIRGO

Thermal noise in the mirror substrates is expected to be the main limit to the VIRGO sensitivity in the 50–500 Hz frequency range. The mechanical quality of the mirror substrates and the geometry of their suspension are expected to affect the noise level of the detector output. High mechanical Q have been obtained for different large fused silica substrates under VIRGO suspension conditions. Moreover, calcium fluoride substrates are shown to provide a more promising option for the design of future cryogenic, low thermal noise interferometers.

Investigation on mechanical losses in TiO2/SiO2 dielectric coatings

Interferometric gravitational wave detectors use test masses made by large mirrors whose coating is usually made by multiple layers of dielectric materials, most commonly alternating layers of SiO2 (silica) and Ta2O5 (tantala). It is foreseeable that in future interferometric gravitational wave detector projects (LCGT, EGO, VIRGO,), the mirrors will be cooled down to cryogenic temperature in order to reduce the noise generated by the thermally activated motion of the masses. However, low temperature mechanical losses in the Ta2O5/SiO2 coatings might limit the design sensitivity for such cryogenic detectors by setting a lower limit for the expected thermal noise. Here we present some measurements of mechanical losses in the TiO2/SiO2 coatings at room and low temperature (80K-300K).

Measurement of the thermoelastic properties of crystalline Si fibres

In order to reduce the thermal noise in future interferometers for gravitational wave (GW) detectors, new suspension materials with low thermal noise are under investigation. Crystalline silicon seems to be a promising material mainly at low temperature. A new technology to produce crystalline silicon fibres has been realized. Measurements of mechanical and thermal properties of the fibres at room temperature have been performed. Preliminary measurements at low temperature are presented.