A kinetic study of the decomposition of benzoyl peroxide assisted by Lewis acids

Sivaram, Swaminathan; Singhal, R. K.; Bhardwaj, I. S.

doi:10.1007/bf00263202

Cited by 14 publications

(12 citation statements)

References 17 publications

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“…A similar test of the WEP for GWs using line of sight Shapiro delay from a GRB, which simultaneously emits GWs and photons was first proposed by Sivaram [31]. All previous detections by LIGO [32][33][34][35] were binary black hole mergers, for which no EM counterparts are expected (See, however [36].)…”

Section: Introductionmentioning

confidence: 80%

GW170817 falsifies dark matter emulators

et al. 2018

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the LIGO interferometers detected the gravitational wave (GW) signal (GW170817) from the coalescence of binary neutron stars. This signal was also simultaneously seen throughout the electromagnetic (EM) spectrum from radio waves to gamma-rays. We point out that this simultaneous detection of GW and EM signals rules out a class of modified gravity theories, termed "dark matter emulators," which dispense with the need for dark matter by making ordinary matter couple to a different metric from that of GW. We discuss other kinds of modified gravity theories which dispense with the need for dark matter and are still viable. This simultaneous observation also provides the first observational test of Einstein's Weak Equivalence Principle (WEP) between gravitons and photons. We estimate the Shapiro time delay due to the gravitational potential of the total dark matter distribution along the line of sight (complementary to the calculation in [1]) to be about 400 days. Using this estimate for the Shapiro delay and from the time difference of 1.7 seconds between the GW signal and gamma-rays, we can constrain violations of WEP using the parameterized post-Newtonian (PPN) parameter γ, and is given by |γGW − γEM| < 9.8 × 10 −8 .

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Section: Introductionmentioning

confidence: 80%

GW170817 falsifies dark matter emulators

et al. 2018

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“…In the framework of parameterized post-Newtonian approximation, deviations from EEP can be described by a parameter γ, which is 1 in general relativity. Therefore, the GW/GRB association is very suitable to test the EEP violation (Sivaram 1999;Wu et al 2016;Li et al 2016a). The Shapiro delay is generally calculated as ∆t gra = − ∆γ c 3 r e r o U(r(t); t) (Shapiro 1964;Krauss & Tremaine 1988;Longo 1988), where the integral is along the travelling path of photons and U(r(t); t) is the gravitational potential.…”

Section: Testing the Einstein Equivalence Principlementioning

confidence: 99%

The GW170817/GRB 170817A/AT 2017gfo Association: Some Implications for Physics and Astrophysics

Wang

Zhang

Wang

et al. 2017

ApJL

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On 17 August 2017, a gravitational wave event (GW170817) and an associated short gamma-ray burst (GRB 170817A) from a binary neutron star merger had been detected. The followup optical/infrared observations also identified the macronova/kilonova emission (AT2017gfo). In this work we discuss some implications of the remarkable GW170817/GRB 170817A/AT2017gfo association. We show that the ∼ 1.7s time delay between the gravitational wave (GW) and GRB signals imposes very tight constraint on the superluminal movement of gravitational waves (i.e., the relative departure of GW velocity from the speed of light is ≤ 4.3 × 10 −16 ) or the possible violation of weak equivalence principle (i.e., the difference of the gamma-ray and GW trajectories in the gravitational field of the galaxy and the local universe should be within a factor of ∼ 3.4 × 10 −9 ). The socalled Dark Matter Emulators and a class of contender models for cosmic acceleration ("Covariant Galileon") are ruled out, too. The successful identification of Lanthanide elements in the macronova/kilonova spectrum also excludes the possibility that the progenitors of GRB 170817A are a binary strange star system. The high neutron star merger rate (inferred from both the local sGRB data and the gravitational wave data) together with the significant ejected mass strongly suggest that such mergers are the prime sites of heavy r-process nucleosynthesis.

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“…In the absence of GW observations, the identification of macronova/kilonova signals in the afterglow of a few short/long-short GRBs provides the strongest support to their compact object merger origin (see Jin et al 2016, and the references therein). The GW/GRB/macronova association provides a wealth of physical information about the source(s) and allows novel tests of fundamental physics (e.g., Sivaram 1999;Del Pozzo et al 2013;Li et al 2016;Miller 2016;Wu et al 2016;Paschalidis 2017), as demonstrated in the case of GW170817/GRB 170817A/AT2017gfo (e.g., Abbott et al 2017c;Wang et al 2017). Moreover, with the increasing sensitivities of the LIGO/Virgo/KAGRA detectors, the number of events will accumulate considerably in the next few years, reliable statistical studies will become possible.…”

Section: Introductionmentioning

confidence: 99%

Black Hole Mass Function of Coalescing Neutron Star Black Hole Binary Systems: The Prospect of Reconstruction with the Gravitational Wave Observations

Tang

Wang

Wang³

et al. 2020

ApJ

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The discovery of gravitational waves from compact objects coalescence opens a brand-new window to observe the universe. With more events being detected in the future, statistical examinations would be essential to better understand the underlying astrophysical processes. In this work we investigate the prospect of measuring the mass function of black holes that are merging with the neutron stars. Applying Bayesian parameter estimation for hundreds of simulated neutron star-black hole (NSBH) mergers, we find that the parameters for most of the injected events can be well recovered. We also take a Bayesian hierarchical model to reconstruct the population properties of the masses of black holes, in the presence of a low mass gap, both the mass gap and power-law index (α) of black hole mass function can be well measured, thus we can reveal where the α is different for binary black hole (BBH) and NSBH systems. In the absence of a low mass gap, the gravitational wave data as well as the electromagnetic data can be used to pin down the nature of the merger event and then measure the mass of these very light black holes. However, as a result of the misclassification of BBH into NSBH, the measurement of α is more challenging and further dedicated efforts are needed.

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A kinetic study of the decomposition of benzoyl peroxide assisted by Lewis acids

Cited by 14 publications

References 17 publications

GW170817 falsifies dark matter emulators

GW170817 falsifies dark matter emulators

The GW170817/GRB 170817A/AT 2017gfo Association: Some Implications for Physics and Astrophysics

Black Hole Mass Function of Coalescing Neutron Star Black Hole Binary Systems: The Prospect of Reconstruction with the Gravitational Wave Observations

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