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Bhaskar Biswas (Universität Hamburg)Gravitational WavesOral
Despite its elegance, the theory of General Relativity is subject to experimental, observational, and theoretical scrutiny to arrive at tighter constraints or an alternative, more preferred theory. In alternative gravity theories, the macroscopic properties of neutron stars, such as mass, radius, tidal deformability, etc. are modified. This creates a degeneracy between the uncertainties in the...
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Johann FernandesGravitational WavesPoster
Intermediate mass black holes (IMBH) with mass ranges between $100 M_\odot$ to $10^5 M_\odot$ provide a missing link between stellar mass and supermassive black holes. Understanding them provides an insight into galaxy formation as they are considered to be the precursors of supermassive black holes. The high mass of IMBH binaries leads to a short gravitational wave signal duration and...
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Mr Mohit Raj Sah (Tata Institute of Fundamental Research, Mumbai)Gravitational WavesPoster
The astrophysical Stochastic Gravitational Wave Background (SGWB) is the superposition of all the compact binary merger events that go undetected as individual events along with other sources such as supernovae, magnetars, etc. The individual gravitational wave (GW) signals from these events vary over time, depending on the source parameters. The timescale of the individual events along with...
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Swetha Bhagwat (University of Birmingham)Gravitational WavesOral
Binary black hole mergers produce a remnant black-hole in a perturbed state. This then relaxes to form a stable Kerr black hole by emitting gravitational waves, which we call as the ringdown. Ringdowns contain imprints of both strong field linear and non-linear dynamics predicted by the general theory of relativity. Traditionally, we have been using ringdown to test strong-field linear...
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Samanwaya Mukherjee (IUCAA, Pune)Gravitational WavesPoster
Being subject to the tidal field of its companion, each component of a coalescing binary suffers a slow change in its mass (tidal heating) and spin (tidal torquing) during the inspiral and merger. For black holes, these changes are associated with the energy and angular momentum fluxes down their horizons. This effect modifies the inspiral rate of the binary, and consequently, the phase and...
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Abhishek SharmaGravitational WavesPoster
LISA (Laser Interferometer Space Antenna) a planned space-based gravitational wave observatory to be launched in 2034 will be capable of detecting gravitational waves in the milli-Hertz band. Among various sources, LISA will detect the coalescence of massive black hole binaries (MBHBs) with total mass in range $[10^4-10^8] \mathrm{M_\odot}$ up to redshift $\sim$ 10. As such cataclysmic...
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Rajendra Prasad Bhatt (Inter-University Centre for Astronomy and Astrophysics, Pune 411007, India)Gravitational WavesOral
Among various properties of black holes studied so far, their response to an external tidal field remains an especially interesting topic. In our recent work [[arXiv:2306.13627 [gr-qc]][1]], we presented an analytic method for calculating the tidal response function of non-rotating and slowly rotating black holes from the Teukolsky equation in the small frequency and the near horizon limit....
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Mr Debanjan Guha Roy (Birla Institute of Technology & Science Pilani, Hyderabad Campus, Secunderabad, Telangana, India)Gravitational WavesOral
Gravitational wave(GW) astronomy has been maturing rapidly since the first detection of gravitational waves. Already, the current GW detectors have the sensitivity to detect gravitational waves emitted from neutron stars. Next-generation detectors will improve on this, resulting in a golden age of GW astronomy for Neutron Stars(NS). The observed mass of NS is limited to around two times that...
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Mr Tathagata Ghosh (Inter-University Centre for Astronomy and Astrophysics)Gravitational WavesOral
Gravitational waves (GW) from the inspiral of binary compact objects offer a one-step measurement of the luminosity distance to the event, which is essential for estimating the Hubble constant, $H_{0}$, that characterizes the expansion rate of the Universe. However, unlike binary neutron stars, the inspiral of binary black holes is not expected to be accompanied by electromagnetic radiation...
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Sayak Datta (Max Planck Institute for Gravitational Physics (AEI))Gravitational WavesOral
From electromagnetic observations, we know that the supermassive black holes at galactic centers are surrounded by dark and baryonic matter. With the advent of gravitational wave (GW) astronomy, we are poised to probe the details of geometry from where GW gets generated. GWs from binaries containing at least one supermassive black hole will be observed with space-based detector LISA. In such a...
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Ms Sulagna Bhattacharya (Tata Institute of Fundamental Research, Mumbai)Gravitational WavesOral
Dark Matter (DM) is ubiquitous and thus has been proposed to be probed by several terrestrial and celestial detectors. DM particles from the galactic halo can accumulate in Neutron Stars (NS) and transmute them into sub-2.5 solar mass black holes (BH) if the DM particles are heavy, stable, and have feeble but sufficient interactions with nucleons. These BHs are named Transmuted Black Holes...
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SUBHASIS MAITI (PhD Student)Gravitational WavesPoster
In the standard Big Bang model, Reheating follows inflation but precedes Big Bang Nucleosynthesis (BBN), marking the transition from the inflationary epoch to the hot Big Bang. During inflation, the universe expands exponentially due to the inflation field's energy. After inflation, as the field oscillates, it transfers energy to other particles, forming a hot, dense plasma. This phase depends...
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Gopalkrishna Prabhu (Inter-University Centre for Astronomy and Astrophysics)Gravitational WavesPoster
Galactic spinning compact objects (COs) with non-zero ellipticity are expected to be sources of continuous gravitational waves (CGWs). Certain classes of hypothetical compact objects, such as neutron stars with quark cores (hybrid stars), and quark stars, are thought to have large ellipticities from theoretical considerations. These should enable such COs to produce CGWs detectable by the...
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Shailesh KumarGravitational WavesPoster
Aspects related to black holes surrounded by the astrophysical environment are underappreciated and require profound attention and effort. From an astrophysical viewpoint, we know that dark matter is asserted to be an undetected form of an elementary particle that is not visible, does not interact and contributes almost 27% to the matter-energy of the universe. The development of gravitational...
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Ms Mayusree Das (Indian Institute of Science)Gravitational WavesPoster
In the past decades, several neutron stars (NSs), particularly pulsars, with mass $M > 2M_\odot$ have been observed. Hence, there is a generic question of the origin of massive compact objects. Here we explore the existence of massive, magnetized, rotating NSs with various equation of states (EoSs) using XNS code, which solves axisymmetric stationary stellar equilibria in general relativistic...
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GOURAB BANERJEE (SAHA INSTITUTE OF NUCLEAR PHYSICS)Gravitational WavesPoster
Matter inside a neutron star is composed of nucleons in β-equilibrium up to
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2-3 times saturation density(ρ0). The equation of state(EOS) of such matter can
be expressed using iso-scalar and iso-vector nuclear matter parameters (NMPs)
which characterize the symmetric nuclear matter (SNM) and density-dependent
symmetry energy, respectively. The tidal deformation of a neutron star in... -
Soham Bhattacharyya (IIT Madras)Gravitational WavesOral
So far, the post-Newtonian technique has generated spin-less gravitational waveforms of binaries in quasi-circular orbits to a very high degree of precision, or to a high post-Newtonian order. Including spins and eccentricity in the system brings challenges that have not been fully tackled to a high degree of accuracy. The inclusion of spins leads to characteristic effects on the orbital...
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Shamim Haque (Indian Institute of Science Education and Research Bhopal)Gravitational WavesPoster
Quantum chromodynamics predicts that at high enough temperature/density, hadronic matter (HM) deconfines to quark-gluon matter. it is conjectured that the deconfinement transition from HM to quark matter (QM) takes place at an intermediate density range (a few times nuclear matter density). However, there is no ab-initio calculation, nor are there any earth-based experiments. The only...
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Md Emanuel Hoque (Saha Institute of Nuclear Physics)Gravitational WavesPoster
We have investigated the detection probability of continuous Gravitational Wave (CW) signals from the spinning neutron stars in our galaxy across a wide range of their spin frequency. For this purpose, we use observed neutron stars' spin frequencies and spin-down rates, observed with radio telescopes as provided in the Australia Telescope National Facility (ATNF) pulsar catalog. We model the...
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R. Prasad (International Centre for Theoretical Sciences, TIFR, Bangalore)Gravitational WavesPoster
Gravitational waves (GWs) emitted from astrophysical sources can get lensed on their way to Earth, similar to electromagnetic waves. There are claims that detections made by LIGO and Virgo in earlier observational runs show evidence of lensing. Lensing has been invoked to explain the discovered high mass events, the bimodal mass function distribution of black holes, and for the objects in the...
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Abhishek Chowdhuri (IIT Gandhinagar)Gravitational WavesPoster
In this talk we will explore the late inspiral and then the transition regime to the plunge phase of a secondary, less massive compact object into a more massive deformed Kerr black hole. We will show how one can find fluxes such as the energy and the angular momentum and henceforth use them to infer about their detectibility from a GW standpoint. We also explore how the different deviation...
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Dr Rakesh Kabir (University of Delhi)Gravitational WavesOral
The detection and parameter estimation of compact binary coalescences (CBC) through the analysis of gravitational wave signals have been revolutionized by the advent of deep learning neural networks. Conventionally, curriculum learning, a method that progressively exposes a neural network to more challenging examples during training, has emerged as the de facto procedure for training these...
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107. Gear-up for the Action Replay: Leveraging Lensing for Enhanced Gravitational-Wave Early-WarningSourabh Magare (The Inter University Center for Astronomy and Astrophysics)Gravitational WavesOral
Pre-merger gravitational-wave (GW) sky-localisation of binary neutron star (BNS) and neutron star black hole (NSBH) coalescence events, would enable telescopes to capture precursors and electromagnetic (EM) emissions around the time of the merger. We propose an astrophysical scenario that could provide early-warning times of hours to days before coalescence with sub-arcsecond localisation,...
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Susmita JanaGravitational WavesPoster
Correspondence between gravity and other fields in gauge theories is yet to be well understood and experimentally verified. The linearity of other gauge theories(such as Maxwell's theory) and the nonlinearity of general relativity make exploring this realm of gravity quite strenuous. The Gertsenshtein-Zeldovich (GZ) effect belongs to this realm, where electromagnetic (EM) waves passing through...
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Ms Anushka Doke (ICTS-TIFR)Gravitational WavesPoster
We investigate the influence of tidal deformability and strong magnetic fields on the generation of gravitational waves during the inspiral of binary neutron stars in eccentric orbits. Although the current number of identified neutron stars exhibiting strong magnetic fields ($10^{14-15}$ G) remains limited, the maximum allowed magnetic fields in these stars is $10^{18}$ G. Neutron star...
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Dr Surajit Kalita (University of Cape Town)Gravitational WavesPoster
This abstract is primarily based on my recent paper MNRAS 520 (2023) 3742. Since the discovery of fast radio bursts (FRBs), researchers have proposed several theories and models to explain their characteristics. One of the most recent models takes into account the Gertsenshtein-Zel'dovich (GZ) phenomenon, which suggests that a portion of gravitational radiation is converted into...
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Sajal MukherjeeGravitational WavesPoster
In this talk, I will discuss the resonance crossing in an Extreme Mass Ratio Inspiral (EMRI). By assuming a charged particle moving in an external homogeneous magnetic field under the electromagnetic self force (ESF), we discuss how it encounters the resonances. In a past work, we compare the resonance timescale between ESF and its adiabatic counterpart, and obtain a qualitative similarity....
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Mr Pratul Manna (Indian Institute of Technology Madras)Gravitational WavesPoster
In general relativity, eccentricity is not defined uniquely. Different waveform models rely on gauge-dependent definitions of eccentricity and other orbital elements, which leads to incompatibility between different models. We employ a [recently proposed gauge invariant eccentricity definition][1] to eliminate this ambiguity in our PN-NR comparisons. We also present an eccentric GW model by...
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Deeshani Mitra (Summer Student at U²GRC (UMass-URI Gravity Research Consortium))Gravitational WavesPoster
In the domain of gravitational wave exploration, the swift prediction of waveforms holds immense importance for real-time and computational scenarios. Our research revolves around the development of efficient surrogate models, encompassing a three-step process to engineer accurate representations of true waveforms. This endeavour brings about transformative enhancements in waveform prediction,...
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Chandra Kant Mishra (IIT Madras)Gravitational WavesPoster
Post-detection analyses targeting inferences of source properties are often time-consuming and computationally expensive. Assumptions concerning source properties, such as the circularity of binary orbits or the absence of precessing component spins, are routinely made to reduce analysis costs. We shall present a method that may be used to infer the presence (or the lack thereof) of physical...
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Krishnendu N VGravitational WavesOral
We propose a novel test for the quantum nature of astrophysical black holes using gravitational-wave measurements.
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It is known that the black hole absorption and emission spectra will be quantised if the black hole area is quantised. Focusing on the black hole absorption spectra for binary black holes in the pre-merger signal, we quantify the measurability of black hole area quantisation... -
Mr Sachin Shukla (Indian Institute of Technology Gandhinagar)Gravitational WavesPoster
LIGO-Aundha is expected to join the network of terrestrial broadband gravitational wave (GW) detectors and begin operations in the early 2030s. We study the impact of this additional detector on the accuracy of determining the direction of incoming transient signals from coalescing binary neutron star sources. Our study involves performing a full Bayesian parameter estimation (PE) over a...
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Kaustubh Gupta (Indian Institute of Science Education and Research Pune)Gravitational WavesPoster
Measurements of the Cosmic Microwave Background Radiation indicate the presence of a dipole anisotropy in the sky distribution of temperature fluctuations of the CMB photons. It is believed that the CMB dipole arises because of the earth's motion with respect to the cosmic rest-frame; hence, the strength of the dipole provides an estimate of the earth's speed. Similar measurements recently...
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SARBARI GUHA (Associate Professor, Department of Physics, St. Xavier's College (Autonomous), Kolkata 700016, INDIA)Gravitational WavesPoster
In this paper we study the memory effect produced in pp-wave spacetimes due to the passage of gravitational wave pulses. We assume the pulse profile in the form of a ramp (which may be considered as an appropriate representation of burst gravitational waves), and analyse its effects on the evolution of nearby geodesics. For a ramp profile, we are able to determine analytical solutions of the...
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Apratim Ganguly (IUCAA)Gravitational WavesPoster
GR tests used by the LIGO-Virgo-KAGRA collaboration probes various parts of the gravitational-wave signal. However, a comprehensive understanding of the tests requires accounting for potential biases introduced by unmodeled physical effects like eccentricity, spin precession, or lensing. In this talk, we delve into the intricate influence of microlensing and millilensing on the IMR consistency...
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M Laxman (IIT Madras)Gravitational WavesPoster
Most of the gravitational wave (GW) signals detected so far by LIGO and Virgo detectors consist of comparable mass binary black holes (BBHs). Another interesting source of GWs is highly eccentric intermediate mass ratio inspirals (IMRIs). GW signals from IMRI sources are expected to be highly eccentric when they enter the detection band of the space based detectors such as LISA and DECIGO....
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Avinash Kumar Paladi (Indian Institute of Science)Gravitational WavesOral
The wideband timing technique enables the high-precision simultaneous estimation of Times of Arrival (ToAs) and Dispersion Measures (DMs) while effectively modeling frequency-dependent profile evolution. We present two novel independent methods that extend the standard wideband technique to handle simultaneous multi-band pulsar data incorporating profile evolution over a larger frequency span...
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Aman SrivastavaGravitational WavesOral
The Indian Pulsar Timing Array (InPTA) collaboration has recently made its first official data release (DR1) for a sample of 14 pulsars using 3.5 years of uGMRT observations. We present the results of single-pulsar noise analysis for each of these 14 pulsars using the InPTA DR1. For this purpose, we consider white noise, achromatic red noise, dispersion measure (DM) variations, and scattering...
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Andrew MillerGravitational WavesOral
The third observing run of advanced LIGO, Virgo and KAGRA brought unprecedented sensitivity towards a variety of quasi-monochromatic, persistent gravitational-wave signals. Continuous waves allow us to probe not just the canonical asymmetrically rotating neutron stars, but also different forms of dark matter, thus showing the wide-ranging astrophysical implications of using a relatively simple...
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Neev Shah (IISER, Pune & ICTS-TIFR, Bengaluru)Gravitational WavesPoster
Lensing due to intervening matter such as clusters or galaxies can (de)magnify a gravitational-wave (GW) event, leading to a biased measurement of the source mass and redshift. Hierarchical inference on the detected GW events can be performed to estimate the population properties of binary black holes, such as their mass and redshift distributions. Currently, it is assumed that the current...
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Raj Patil (Max Planck Institute for Gravitational Physics (Albert Einstein Institute) and Humboldt University)Gravitational WavesOral
The observations of gravitational waves (GW) have proved to be a probe for the physics of celestial objects like black holes (BH) and neutron stars (NS). Such detections have the potential to unravel the mysteries of cosmic origins, equations of state of compact objects and will prove to be a test of the theory of general relativity. To successfully achieve these scientific goals, it is...
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Uddeepta DekaGravitational WavesPoster
Gravitational lensing of gravitational waves (GW) opens up the exciting possibility of studying the properties of the lens. If the wavelength of GW is comparable to the Einstein radius of the lens, diffraction effects modulate the GW waveform. Previous work has shown that if the lens is a stellar mass Schwarzschild black hole (BH), and the GWs have wavelengths detectable by the...
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AVINASH TIWARI (IUCAA, PUNE)Gravitational WavesOral
The accelerated motion of binary black holes (BBHs) can be constrained by the corresponding gravitational waves (GWs) they emit. We investigate the prospects of detecting this acceleration in future third-generation and proposed space-based GW detectors. Since this acceleration could be indicative of the binary's formation channel, we also forecast accelerations of BBHs in dense stellar...
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Souvik Jana (ICTS-TIFR)Gravitational WavesOral
Third generation gravitational wave (GW) detectors are expected to detect millions of binary black hole (BBH) mergers during their operation period. A small fraction of them (∼1%) will be strongly lensed by intervening galaxies and clusters, producing multiple observable copies of the GW signals. The expected number of lensed events and the distribution of the time delay between lensed images...
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Ms Neha Sharma (International Centre for Theoretical Sciences (ICTS))Gravitational WavesPoster
The lensing of gravitational waves occurs when it passes near massive objects like galaxies and clusters that bends its path. The detection of the first lensed gravitational wave is expected within the next few years. Decihertz detectors such as Lunar Gravitational Wave Antenna (LGWA) are expected to detect gravitational waves from intermediate mass blackhole mergers and white dwarf binaries....
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Alapati Tharaka Rama Chowdary (Indian Institute of Technology, Bombay)Gravitational WavesOral
One of the key aims of next-generation gravitational wave detectors is to test General Relativity (GR) in the strong gravity regime. It is expected that gravity is modified in the strong gravity regime. Hence, it is imperative to obtain rotating black hole solutions in modified theories of gravity, look at their quasinormal mode (QNM) signatures, and obtain the difference between the new...
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Yuvraj SharmaGravitational WavesPoster
The future of Gravitational Wave (GW) detectors [LVK] have made remarkable progress, with an expanding sensitivity band and the promise of exponential increase in detection rates for upcoming observing runs [O4 and beyond]. Among the diverse sources of GW signals, eccentric Binary mergers present an intriguing and computationally challenging aspect. We address the imperative need for efficient...
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Pankaj Saini (Chennai Mathematical Institute)Gravitational WavesPoster
Next generation gravitational wave (GW) detectors are expected to detect $10^4 \mbox{--} 10^5$ binary black holes (BBHs) per year. Understanding the formation pathways of these binaries is an open question. Orbital eccentricity can be used to distinguish between the formation channels of compact binaries as different formation channels are expected to yield distinct eccentricity distributions....
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Mr Rajesh Karmakar (Indian Institute Of Technology, Guwahati)Gravitational WavesPoster
Within the framework of static-charged and rotating black hole spacetime, an extensive amount of work suggests that the bosonic fields exhibit superradiant scattering. In this work, we have investigated the scattering of scalar waves and electromagnetic (EM) waves for Schwarzschild black hole in the ring down phase (we refer to this black hole as the ``ringing black hole"), which is the last...
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Akash Maurya (International Centre for Theoretical Sciences, Bangalore)Gravitational WavesPoster
Orbital eccentricity of coalescing compact binaries produces a strong imprint in the gravitational waves (GWs) emitted by these systems. Its presence indicates at dynamically assembled binaries in dense stellar environments like globular clusters, nuclear star clusters, etc. Hence, detecting an eccentric merger will significantly enhance our knowledge about the formation channels of these...
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Sajad Ahmad Bhat (IUCAA)Gravitational WavesPoster
The parametrized post-Newtonian (PN) test of general relativity (GR) currently assumes binary black holes (BBHs) in quasi-circular orbits. However, population simulations predict that a subpopulation of BBHs retain residual eccentricity in the frequency-band of ground-based detectors. To perform robust parametrized tests of GR with eccentric binaries, corrections due to orbital eccentricity...
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Parthapratim Mahapatra (Chennai Mathematical Institute, LIGO-India Scientific Collaboration (LISC))Gravitational WavesOral
Asymmetric emission of gravitational waves during a compact binary coalescence results in the loss of linear momentum and a corresponding `kick' or recoil on the binary's center of mass. This leads to a direction-dependent Doppler shift of the ringdown gravitational waveform. We quantify the measurability of the kick imparted to the remnant black hole in a binary black hole merger. Future...
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Dr Poulami Dutta Roy (Chennai Mathematical Institute)Gravitational WavesOral
Gravitational-wave observations are unique means to test general relativity (GR) in the strong-field regime. Parametrized tests of post-Newtonian theory have been very efficient in testing GR in the inspiral phase of compact binary dynamics. In this test, one introduces deformation coefficients at each post-Newtonian order in the inspiral phase of the gravitational wave which by definition are...
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Divyajyoti . (Indian Institute of Technology Madras)Gravitational WavesPoster
We investigate the prospect of performing binary black hole (BBH) nature tests using spin-induced multipole moment (SIQM) measurements when the binary is fully precessing. As SIQM is strongly degenerate with spin parameters, we are interested in the degeneracies the SIQM parameter has with spin precession. We extend the previous SIQM-based BBH nature tests by incorporating two-parameter...
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VARENYA UPADHYAYA (Indian Institute of Technology, Hyderabad)Gravitational WavesPoster
Pulsars are fast spinning neutron stars that lose their rotational energy via various processes such as gravitational and magnetic radiation, particle acceleration and mass loss processes. This dissipation can be quantified by a spin-down equation that measures the rate of change of the frequency as a function of the rotational frequency itself. We explore the pulsar spin-down and consider the...
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Vaishak Prasad (International Centre for Theoretical Sciences - Tata Institute of Fundamental Research)Gravitational WavesOral
It is widely believed that in the post-Newtonian approach, the asymptotic gravitational fields of non-spinning black holes do not deform under the influence of its companion. Would their horizons deform? In this talk, we present an alternate approach to the problem of tidal deformations of black holes in binary mergers using the source multipole moments of their dynamical horizons and...
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SUPROVO GHOSHGravitational WavesOral
The cores of neutron stars (NS) reach densities several times the nuclear saturation density and could contain strangeness containing exotic particles such as hyperons. During the binary inspiral, viscous processes inside the NS matter can damp out the tidal energy induced by the companion and convert this to thermal energy to heat up the star. In this work, we demonstrate that the bulk...
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Sayantan Ghosh (Indian Institute of Technology Bombay)Gravitational WavesOral
Intermediate-mass black holes (IMBHs) are considered to be seeds of supermassive black holes (SMBHs). Knowledge of the formation and the growth of IMBHs can lead to a better understanding of SMBH formation and galaxy evolution. In recent years, gravitational waves (GWs) have opened a new window to observe and study IMBHs. The advanced ground-based GW detectors, such as Advanced LIGO and...
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Anuj MishraGravitational WavesPoster
Microlensing and eccentricity are two distinct physical effects that have not yet been observed in real gravitational wave events. While the rate of microlensed signals remains uncertain, the impact of non-zero eccentricity becomes increasingly significant as we explore the early stages of binary evolution or improve the sensitivity of detectors. Therefore, it is crucial to investigate whether...
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Kaushik Paul (Indian Institute of Technology Madras)Gravitational WavesOral
The network of LIGO-Virgo detectors has detected nearly 100 compact binary mergers in their three observing runs, among which most of the merger events are from quasicircular orbits. Though binaries tend to circularize when they enter the LIGO band, binaries formed via dynamical interactions in dense stellar clusters or through Kozai-Lidov processes can have large residual eccentricities. As...
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