Gravitational radiation from the Galaxy

Hils, D.; Bender, P. L.; Webbink, R. F.

doi:10.1086/169098

Cited by 254 publications

(351 citation statements)

References 0 publications

Supporting

Mentioning

343

Contrasting

Order By: Relevance

“…(3,4,5), cannot be written (to our knowledge) in closed analytic form. However, by using the LWL expansion of the X GW -response, it is possible to obtain a closed-form expression of its Fourier transform.…”

Section: A the Fourier Transform Of A Binary Signalmentioning

confidence: 98%

“…The coefficients (a (1) , a (2) , a (3) , a (4) ) depend only on the two independent amplitudes of the gravitational wave signal, (h + , h × ), the polarization angle, ψ, and an arbitrary phase, φ 0 , that the signal has at time t = 0. Their analytic expressions are given in equations (41-44) of reference [8], while the functions u k (t), and v k (t) (k = 2, 3) are given in equations (27,28) in the same reference.…”

Section: The Lisa Response To Signals From Binary Systemsmentioning

confidence: 99%

“…For details on this simulation we refer the reader to [18], and for earlier work to [2,3,4,19,20,21]. The basic ingredient for these simulations is an approximate binary evolution code.…”

Section: White Dwarf Binary Population Distributionmentioning

confidence: 99%

“…It has been shown in the literature (see [2] for a recent study and [3,4] for earlier investigations) that these sources will be dominated by detached white-dwarf -white-dwarf (WD-WD) binaries, with 1.1 × 10 8 of such systems in our Galaxy. The detached WD-WD binaries evolve by gravitational-radiation reaction and the number of such sources rapidly decreases with increasing orbital frequency.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

White-dwarf–white-dwarf galactic background in the LISA data

et al. 2005

View full text Add to dashboard Cite

LISA (Laser Interferometer Space Antenna) is a proposed space mission, which will use coherent laser beams exchanged between three remote spacecraft to detect and study low-frequency cosmic gravitational radiation. In the low-part of its frequency band, the LISA strain sensitivity will be dominated by the incoherent superposition of hundreds of millions of gravitational wave signals radiated by inspiraling white-dwarf binaries present in our own galaxy. In order to estimate the magnitude of the LISA response to this background, we have simulated a synthesized population that recently appeared in the literature. Our approach relies on entirely analytic expressions of the LISA Time-Delay Interferometric responses to the gravitational radiation emitted by such systems, which allows us to implement a computationally efficient and accurate simulation of the background in the LISA data. We find the amplitude of the galactic white-dwarf binary background in the LISA data to be modulated in time, reaching a minimum equal to about twice that of the LISA noise for a period of about two months around the time when the Sun-LISA direction is roughly oriented towards the Autumn equinox. This suggests that, during this time period, LISA could search for other gravitational wave signals incoming from directions that are away from the galactic plane. Since the galactic white-dwarfs background will be observed by LISA not as a stationary but rather as a cyclostationary random process with a period of one year, we summarize the theory of cyclostationary random processes, present the corresponding generalized spectral method needed to characterize such process, and make a comparison between our analytic results and those obtained by applying our method to the simulated data. We find that, by measuring the generalized spectral components of the white-dwarf background, LISA will be able to infer properties of the distribution of the white-dwarfs binary systems present in our Galaxy.

show abstract

Section: A the Fourier Transform Of A Binary Signalmentioning

confidence: 98%

Section: The Lisa Response To Signals From Binary Systemsmentioning

confidence: 99%

“…For details on this simulation we refer the reader to [18], and for earlier work to [2,3,4,19,20,21]. The basic ingredient for these simulations is an approximate binary evolution code.…”

Section: White Dwarf Binary Population Distributionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

White-dwarf–white-dwarf galactic background in the LISA data

et al. 2005

View full text Add to dashboard Cite

show abstract

“…Following the convention adopted in the LISA community, the detectability threshold was settled to be S/N = 5 and from the numerical solution of eq.21 one obtains, for a given compact object of mass m co , the maximum redshift as function of the SMBH mass M bh . The effective noise budget sensitivity (see eq.16) used in the calculations refers to a standard Michelson configuration [34], including the contribution of the galactic binary WD-WD confusion noise [35,36]. The resulting curves for white dwarfs (m wd = 0.7 M ⊙ ), neutron stars (m ns = 1.4 M ⊙ ) and stellar black holes (m bh = 10 M ⊙ ) are shown in fig.3.…”

Section: The Redshift Space Probed By Lisamentioning

confidence: 99%

Capture rates of compact objects by supermassive black holes

Pacheco

Filloux²,

Regimbau³

2006

Phys. Rev. D

View full text Add to dashboard Cite

Capture rates of compact objects were calculated by using a recent solution of the Fokker-Planck equation in energy-space, including two-body resonant effects. The fraction of compact objects (white dwarfs, neutron stars and stellar black holes) was estimated as a function of the luminosity of the galaxy from a new grid of evolutionary models. Stellar mass densities at the influence radius of central supermassive black holes were derived from brightness profiles obtained by Hubble Space Telescope observations. The present study indicates that the capture rates scale as ∝ M −1.048 bh , consequence of the fact that dwarf galaxies have denser central regions than luminous objects. If the mass distribution of supermassive black holes has a lower cutoff at ∼ 1.4×10 6 M⊙ (corresponding to the lowest observed supermassive black hole mass, located in M32), then 9 inspiral events are expected to be seen by LISA (7-8 corresponding to white dwarf captures and 1-2 to neutron star and stellar black hole captures) after one year of operation. However, if the mass distribution extends down to ∼ 2 × 10 5 M⊙, then the total number of expected events increases up to 579 (corresponding to ∼ 274 stellar black hole captures, ∼ 194 neutron star captures and ∼ 111 white dwarf captures).

show abstract

On the feasibility of employing solar‐like oscillators as detectors for the stochastic background of gravitational waves

Siegel

Roth

2012

Astron Nachr

View full text Add to dashboard Cite

We present a hydrodynamic model that describes excitation of linear stellar oscillations by a stochastic background of gravitational waves (SBGW) of astrophysical and cosmological origin. We find that this excitation mechanism is capable of generating solar g-mode amplitudes close to or comparable with values expected from excitation by turbulent convection, which is considered to be the main driving force for solar-like oscillations. A method is presented that places direct upper bounds on the SBGW in a frequency range, in which the SBGW is expected to contain rich astrophysical information. Employing estimates for solar g-mode amplitudes, the proposed method is demonstrated to have the potential to compete with sensitivities reached by gravitational wave experiments in other frequency ranges.

show abstract

Gravitational radiation from the Galaxy

Cited by 254 publications

References 0 publications

White-dwarf–white-dwarf galactic background in the LISA data

White-dwarf–white-dwarf galactic background in the LISA data

Capture rates of compact objects by supermassive black holes

On the feasibility of employing solar‐like oscillators as detectors for the stochastic background of gravitational waves

Contact Info

Product

Resources

About