The gravitational wave signal from the Galactic disk population of binaries containing two compact objects.

By G. Nelemans, Lev Yungelson, S. P. Portegies Zwart. 2001

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We review the properties of Galactic binaries containing two compact objects, as derived by means of population synthesis. Using this information we calculate the gravitational wave signal of these binaries. At frequencies below f < 2 mHz the double white dwarf population forms an unresolved background for the low- frequency gravitational wave detector LISA. Above this limit some few thousand double white dwarfs and few tens of binaries containing neutron stars will be resolved. Of the resolved double white dwarfs500 have a total mass above the Chandrasekhar limit. About95 of these have a measurable frequency change allowing a determination of their chirp mass. We discuss the properties of the resolved systems.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/f15fb119d986b16b00fdf8f218b2f608ad73d68b

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In Astronomy and Astrophysics

In Atomic and Molecular Physics, and Optics

Citations in the corpus

ASTROPHYSICAL IMPLICATIONS OF THE BINARY BLACK HOLE MERGER GW150914 (2016, background): “The existence of GW150914 shows that BBH mergers occur in nature, and therefore models that do not predict their existence within a Hubble time through any formation channel are excluded(e.g., certain models in Nelemans et al. 2001; Belczynski et al. 2002, 2007; Mennekens & Vanbeveren 2014).”
RATES AND DELAY TIMES OF TYPE Ia SUPERNOVAE (2009, background): “On the other hand, it has been suggested that the SFR of the MW has been decreasing with time, only reaching ∼ 3.5 M yr−1 at the current epoch (Nelemans et al. 2001, 2004, see sect.”
Short-period AM CVn systems as optical, X-ray and gravitational-wave sources (2003, methodology): “One has to keep in mind that a lot of these assumptions are badly constrained, which means that the number of progenitor systems is rather uncertain (e.g. Nelemans et al. 2001a).”
LISA verification binaries with updated distances from Gaia Data Release 2 (2018, methodology): “The catalog was obtained using the binary population synthesis model of Nelemans et al. (2001a); Toonen et al. (2017) and designed to test the detectability of these binaries by Gaia, LSST and LISA.”
COSMOLOGICAL FAST RADIO BURSTS FROM BINARY WHITE DWARF MERGERS (2013, methodology): “Finally, gravitational waves from binary WDs in the in-spiral and merger phase should be detectable by LISA and DECIGO (Nelemans et al. 2001; Farmer & Phinney 2003).”
COSMIC Variance in Binary Population Synthesis (2019, methodology): “We find that the number of resolved DWDs from our simulations is in agreement within a factor of ∼ 2 Nelemans et al. (2001); Ruiter et al. (2010); Nissanke et al. (2012); Korol et al. (2017); Lamberts et al. (2019), however we note that we find relatively more He + He than CO + He DWDs than…”
DOUBLE COMPACT OBJECTS. III. GRAVITATIONAL-WAVE DETECTION RATES (2015, neutral): “…in the past decade (e.g., Lipunov et al. 1997; Bethe & Brown 1998; De Donder & Vanbeveren 1998, 2004a; Bloom et al. 1999; Grishchuk et al. 2001; Nelemans et al. 2001; Dewi & Pols 2003; Voss & Tauris 2003a; Nutzman et al. 2004; Pfahl et al. 2005; Postnov & Yungelson 2006; Marassi et al. 2011;…”
The gravitational wave background from cosmological compact binaries (2003, methodology): “…not attempt to compare to distributions in mass, mass ratio or period in detail: the observed distributions are subject to complex selection effects, and turn out often to be most constraining for WD cooling models (e.g. Nelemans et al. 2001b), whose development is beyond the scope of this paper.”
Prospects for detection of detached double white dwarf binaries with Gaia, LSST and LISA (2017, methodology): “To obtain a model sample of the Galactic DWD population, we use the binary population synthesis code SEBA, developed by Portegies Zwart & Verbunt (1996, for updates see Nelemans et al. 2001a, Toonen et al. 2012).”
The effect of pair-instability mass loss on black-hole mergers (2016, background): “More recently, a number of groups have provided evolutionary models leading to potential BH-BH formation in a typical Galactic environment with high metallicity stars (Brown et al. 2001; Nelemans et al. 2001; Belczynski et al. 2002; Voss & Tauris 2003; Postnov & Yungelson 2006).”
The imprint of massive black hole formation models on the LISA data stream (2007, background): “…obtained by adding in quadrature the instrumental rms noise (given by e.g. the Larson’s online sensitivity curve generator http://www.srl.caltech.edu/∼shane/sensitivity) and the confusion noise from unresolved galactic (Nelemans et al. 2001) and extragalactic (Farmer & Phinney 2003) WD–WD binaries.”
Taiji program: Gravitational-wave sources (2018, background): “The population of compact binaries is calculated in [19].”
Physics, Astrophysics and Cosmology with Gravitational Waves (2009, background): “[272] estimate that the effective noise power contributed by binaries in the galaxy is”