scholarly journals Degeneracy between mass and peculiar acceleration for the double white dwarfs in the LISA band

2021 ◽  
Vol 502 (3) ◽  
pp. 4199-4209
Author(s):  
Zeyuan Xuan ◽  
Peng Peng ◽  
Xian Chen

ABSTRACT Mass and distance are fundamental quantities to measure in gravitational wave (GW) astronomy. However, recent studies suggest that the measurement may be biased due to the acceleration of GW source. Here, we develop an analytical method to quantify such a bias induced by a tertiary star on a double white dwarf (DWD), since DWDs are the most common GW sources in the milli-Hertz band. We show that in a large parameter space the mass is degenerate with the peculiar acceleration, so that from the waveform we can only retrieve a mass of ${\cal M}(1+\Gamma)^{3/5}$, where ${\cal M}$ is the real chirp mass of the DWD and Γ is a dimensionless factor proportional to the peculiar acceleration. Based on our analytical method, we conduct mock observation of DWDs by the Laser Interferometer Space Antenna. We find that in about $9{{\ \rm per\ cent}}$ of the cases the measured chirp mass is biased by $(5-30){{\ \rm per\ cent}}$ due to the presence of a tertiary. Even more extreme biases are found in about a dozen DWDs and they may be misclassified as double neutron stars, binary black holes, DWDs undergoing mass transfer, or even binaries containing lower-mass-gap objects and primordial black holes. The bias in mass also affects the measured distance, resulting in a seemingly overdensity of DWDs within a heliocentric distance of 1 kpc as well as beyond 100 kpc. Our result highlights the necessity of modelling the astrophysical environments of GW sources to retrieve their correct physical parameters.

2021 ◽  
Vol 104 (8) ◽  
Author(s):  
B. O’Brien ◽  
M. Szczepańczyk ◽  
V. Gayathri ◽  
I. Bartos ◽  
G. Vedovato ◽  
...  

2020 ◽  
Vol 124 (7) ◽  
Author(s):  
Antonios Tsokaros ◽  
Milton Ruiz ◽  
Stuart L. Shapiro ◽  
Lunan Sun ◽  
Kōji Uryū

2020 ◽  
Vol 497 (1) ◽  
pp. 1043-1049 ◽  
Author(s):  
Ugo N Di Carlo ◽  
Michela Mapelli ◽  
Yann Bouffanais ◽  
Nicola Giacobbo ◽  
Filippo Santoliquido ◽  
...  

ABSTRACT Pair instability (PI) and pulsational PI prevent the formation of black holes (BHs) with mass ≳60 M⊙ from single star evolution. Here, we investigate the possibility that BHs with mass in the PI gap form via stellar mergers and multiple stellar mergers, facilitated by dynamical encounters in young star clusters. We analyse 104 simulations, run with the direct N-body code nbody6++gpu coupled with the population synthesis code mobse. We find that up to ∼6 per cent of all simulated BHs have mass in the PI gap, depending on progenitor’s metallicity. This formation channel is strongly suppressed in metal-rich (Z = 0.02) star clusters because of stellar winds. BHs with mass in the PI gap are initially single BHs but can efficiently acquire companions through dynamical exchanges. We find that ∼21 per cent, 10 per cent, and 0.5 per cent of all binary BHs have at least one component in the PI mass gap at metallicity Z = 0.0002, 0.002, and 0.02, respectively. Based on the evolution of the cosmic star formation rate and metallicity, and under the assumption that all stars form in young star clusters, we predict that ∼5 per cent of all binary BH mergers detectable by advanced LIGO and Virgo at their design sensitivity have at least one component in the PI mass gap.


2020 ◽  
Vol 897 (1) ◽  
pp. 100 ◽  
Author(s):  
L. A. C. van Son ◽  
S. E. De Mink ◽  
F. S. Broekgaarden ◽  
M. Renzo ◽  
S. Justham ◽  
...  

2020 ◽  
Vol 102 (4) ◽  
Author(s):  
Vishal Baibhav ◽  
Davide Gerosa ◽  
Emanuele Berti ◽  
Kaze W. K. Wong ◽  
Thomas Helfer ◽  
...  

2021 ◽  
Vol 910 (1) ◽  
pp. 30
Author(s):  
Ataru Tanikawa ◽  
Hajime Susa ◽  
Takashi Yoshida ◽  
Alessandro A. Trani ◽  
Tomoya Kinugawa

1985 ◽  
Vol 145 (3) ◽  
pp. 369 ◽  
Author(s):  
A.G. Polnarev ◽  
M.Yu. Khlopov

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