Measuring parity violation in the Stochastic Gravitational Wave Background with the LISA-Taiji network

Orlando, Giorgio; Pieroni, Mauro; Ricciardone, Angelo

doi:10.1088/1475-7516/2021/03/069

Cited by 57 publications

(52 citation statements)

References 67 publications

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“…[79]. The potential detection of polarization can be improved by cross-correlating two space-based GW detectors as, for example, LISA and Taiji, or LISA and TianQin [80]. We show that the circular degree of polarization computed from direct numerical simulations follows the HT turbulence model of previous analytical works if the magnetic field is assumed to be present at the initial time of generation.…”

mentioning

confidence: 63%

“…Hence, a priori, parity violating effects cannot be detected if the system of GW detectors is coplanar, which is the case for space-based GW detectors, and the GW background is isotropic [103]. However, different approaches have recently been proposed to detect the circular polarization of a statistically isotropic GW background [79,80]. On the one hand, a statistically isotropic GW background, such as that expected from cosmological sources, can present anisotropies that have been kinematically induced due to the proper motion of the solar system, and the induced anisotropies allow to detect the circular polarization of the background [66,67].…”

Section: Interferometry Of Gw Detectors Lisa and Taijimentioning

confidence: 99%

“…This has been considered in the case of ground-based GW detectors; see, e.g., refs. [79,[103][104][105][106], and for the LISA-Taiji network [80].…”

Section: Interferometry Of Gw Detectors Lisa and Taijimentioning

confidence: 99%

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Polarization of gravitational waves from helical MHD turbulent sources

Pol,

Mandal,

Brandenburg

et al. 2021

Preprint

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We use direct numerical simulations of decaying primordial hydromagnetic turbulence with helicity to compute the resulting gravitational wave (GW) production and its degree of circular polarization. The turbulence is sourced by magnetic fields that are either initially present or driven by an electromotive force applied for a short duration, given as a fraction of one Hubble time. In both types of simulations, we find a clear dependence of the polarization of the resulting GWs on the fractional helicity of the turbulent source. We find a low frequency tail below the spectral peak shallower than the f 3 scaling expected at super-horizon scales, in agreement with similar recent numerical simulations. This type of spectrum facilitates its observational detection with the planned Laser Interferometer Space Antenna (LISA). We show that driven magnetic fields produce GWs more efficiently than magnetic fields that are initially present, leading to larger spectral amplitudes, and to modifications of the spectral shape. In particular, we observe a sharp drop of GW energy above the spectral peak that is in agreement with the previously obtained results. The helicity does not have a huge impact on the maximum spectral amplitude in any of the two types of turbulence considered. However, the GW spectrum at wave numbers away from the peak becomes smaller for larger values of the magnetic fractional helicity. Such variations of the spectrum are most noticeable when magnetic fields are driven. The degree of circular polarization approaches zero at frequencies below the peak, and reaches its maximum at the peak. At higher frequencies, it stays finite if the magnetic field is initially present, and it approaches zero if it is driven. We predict that the spectral peak of the GW signal can be

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confidence: 63%

Section: Interferometry Of Gw Detectors Lisa and Taijimentioning

confidence: 99%

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Polarization of gravitational waves from helical MHD turbulent sources

Pol,

Mandal,

Brandenburg

et al. 2021

Preprint

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“…We conclude by mentioning that our analysis is specific to the LISA mission, and a similar study, which could also include cross-correlations [40][41][42], can be undertaken for the Taiji observatory [43], which is projected to be also sensitive to the mHz range like LISA. The mHz range broadly corresponds to features during inflation that occur some ∼ 30 e-folds after the CMB modes have exited the horizon, see e.g.…”

Section: Discussionmentioning

confidence: 99%

Detecting primordial features with LISA

Fumagalli,

Pieroni,

Renaux-Petel

et al. 2021

Preprint

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Oscillations in the frequency profile of the stochastic gravitational wave background are a characteristic prediction of small-scale features during inflation. In this paper we present a first investigation of the detection prospects of such oscillations with the upcoming space-based gravitational wave observatory LISA. As a proof of principle, we show for a selection of feature signals that the oscillations can be reconstructed with LISA, employing a method based on principal component analysis. We then perform a Fisher forecast for the parameters describing the oscillatory signal. For a sharp feature we distinguish between the contributions to the stochastic gravitational wave background induced during inflation and in the post-inflationary period, which peak at different frequencies. We find that for the latter case the amplitude of the oscillation is expected to be measurable with < 10% accuracy if the corresponding peak satisfies h 2 Ω GW 10 −12 -10 −11 , while for inflationary-era gravitational waves a detection of the oscillations requires a higher peak amplitude of h 2 Ω GW , as the oscillations only appear on the UV tail of the spectrum. For a resonant feature the detection prospects with LISA are maximised if the frequency of the oscillation falls into the range ω log = 4 to 10. Our results confirm that oscillations in the frequency profile of the stochastic gravitational wave background are a worthwhile target for future detection efforts and offer a key for experimentally testing inflation at small scales.

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“…During the same period, Chinese space-based GW detectors Taiji [11][12][13] [proposed by the Chinese Academy of Sciences (CAS)] and TianQin [17][18][19] (proposed by the Sun Yat-Sen University (SYSU)) will be launched. The synergic operation of these GW networks would contribute greatly on cosmology and the test of GR [528,559,[561][562][563][564][565][566].…”

Section: -15mentioning

confidence: 99%

The Gravitational-wave physics II: Progress

Bian

Cai

Cao

et al. 2021

Sci. China Phys. Mech. Astron.

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It has been a half-decade since the first direct detection of gravitational waves, which signifies the coming of the era of the gravitational-wave astronomy and gravitational-wave cosmology. The increasing number of the detected gravitational-wave events has revealed the promising capability of constraining various aspects of cosmology, astronomy, and gravity. Due to the limited space in this review article, we will briefly summarize the recent progress over the past five years, but with a special focus on some of our own work for the Key Project "Physics associated with the gravitational waves" supported by the National Natural Science Foundation of China. In particular, (1) we have presented the mechanism of the gravitational-wave production during some physical processes of the early Universe, such as inflation, preheating and phase transition, and the cosmological implications of gravitational-wave measurements; (2) we have put constraints on the neutron star maximum mass according to GW170817 observations; (3) we have developed a numerical relativity algorithm based on the finite element method and a waveform model for the binary black hole coalescence along an eccentric orbit.

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Measuring parity violation in the Stochastic Gravitational Wave Background with the LISA-Taiji network

Cited by 57 publications

References 67 publications

Polarization of gravitational waves from helical MHD turbulent sources

Polarization of gravitational waves from helical MHD turbulent sources

Detecting primordial features with LISA

The Gravitational-wave physics II: Progress

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