SIMBAD references

2010ApJ...715L.138B - Astrophys. J., 715, L138-L141 (2010/June-1)

The effect of metallicity on the detection prospects for gravitational waves.


Abstract (from CDS):

Data from the Sloan Digital Sky Survey (∼300,000 galaxies) indicate that recent star formation (within the last 1 billion years) is bimodal: half of the stars form from gas with high amounts of metals (solar metallicity) and the other half form with small contribution of elements heavier than helium (∼10%-30% solar). Theoretical studies of mass loss from the brightest stars derive significantly higher stellar-origin black hole (BH) masses (∼30-80 M) than previously estimated for sub-solar compositions. We combine these findings to estimate the probability of detecting gravitational waves (GWs) arising from the inspiral of double compact objects. Our results show that a low-metallicity environment significantly boosts the formation of double compact object binaries with at least one BH. In particular, we find the GW detection rate is increased by a factor of 20 if the metallicity is decreased from solar (as in all previous estimates) to a 50-50 mixture of solar and 10% solar metallicity. The current sensitivity of the two largest instruments to neutron star-neutron star (NS-NS) binary inspirals (VIRGO: ∼9 Mpc; LIGO: ∼18) is not high enough to ensure a first detection. However, our results indicate that if a future instrument increased the sensitivity to ∼50-100 Mpc, a detection of GWs would be expected within the first year of observation. It was previously thought that NS-NS inspirals were the most likely source for GW detection. Our results indicate that BH-BH binaries are ∼25 times more likely sources than NS-NS systems and that we are on the cusp of GW detection.

Abstract Copyright:

Journal keyword(s): binaries: close - gravitation - stars: evolution - stars: neutron

Simbad objects: 4

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2010ApJ...715L.138B and select 'bookmark this link' or equivalent in the popup menu


© Université de Strasbourg/CNRS

    • Contact