scholarly journals Multimessenger Probes of High-energy Sources

2019 ◽  
Vol 209 ◽  
pp. 01036
Author(s):  
Dafne Guetta
Keyword(s):  
Gravitational Wave ◽  
Gravitational Waves ◽  
Large Scale ◽  
High Energy ◽  
Compact Objects ◽  
Binary Black Holes ◽  
Comprehensive Picture ◽  
Electromagnetic Signals ◽  
Combine Information ◽  
Open Question

Multimessenger observations may hold the key to learn about the most energetic sources in the universe. The recent construction of large scale observatories opened new possibilities in testing non thermal cosmic processes with alternative probes, such as high energy neutrinos and gravitational waves. We propose to combine information from gravitational wave detections, neutrino observations and electromagnetic signals to obtain a comprehensive picture of some of the most extreme cosmic processes. Gravitational waves are indicative of source dynamics, such as the formation, evolution and interaction of compact objects. These compact objects can play an important role in astrophysical particle acceleration, and are interesting candidates for neutrino and in general high-energy astroparticle studies. In particular we will concentrate on the most promising gravitational wave emitter sources: compact stellar remnants. The merger of binary black holes, binary neutron stars or black hole-neutron star binaries are abundant gravitational wave sources and will likely make up the majority of detections. However, stellar core collapse with rapidly rotating core may also be significant gravitational wave emitter, while slower rotating cores may be detectable only at closer distances. The joint detection of gravitational waves and neutrinos from these sources will probe the physics of the sources and will be a smoking gun of the presence of hadrons in these objects which is still an open question. Conversely, the non-detection of neutrinos or gravitational waves from these sources will be fundamental to constrain the hadronic content.

scholarly journals Electromagnetic counterparts of compact binary mergers

2021 ◽  
Vol 87 (1) ◽  
Author(s):  
Stefano Ascenzi ◽  
Gor Oganesyan ◽  
Marica Branchesi ◽  
Riccardo Ciolfi
Keyword(s):  
Gravitational Waves ◽  
High Energy ◽  
Design Sensitivity ◽  
Compact Objects ◽  
Open Problems ◽  
Binary Neutron Star ◽  
Compact Binary ◽  
Open Questions ◽  
Binary Mergers ◽  
Electromagnetic Signals

The first detection of a binary neutron star merger through gravitational waves and photons marked the dawn of multimessenger astronomy with gravitational waves, and it greatly increased our insight in different fields of astrophysics and fundamental physics. However, many open questions on the physical process involved in a compact binary merger still remain and many of these processes concern plasma physics. With the second generation of gravitational wave interferometers approaching their design sensitivity, the new generation under design study and new X-ray detectors under development, the high energy universe will become more and more a unique laboratory for our understanding of plasma in extreme conditions. In this review, we discuss the main electromagnetic signals expected to follow the merger of two compact objects highlighting the main physical processes involved and some of the most important open problems in the field.

scholarly journals High-energy astrophysics and the search for sources of gravitational waves

2018 ◽  
Vol 376 (2120) ◽  
pp. 20170294 ◽  
Author(s):  
P. T. O'Brien ◽  
P. Evans
Keyword(s):  
Gravitational Wave ◽  
Short Duration ◽  
Gamma Ray ◽  
New Technology ◽  
High Energy ◽  
Compact Objects ◽  
Wide Field ◽  
High Energy Radiation ◽  
Energy Radiation ◽  
Binary Mergers

The dawn of the gravitational-wave (GW) era has sparked a greatly renewed interest into possible links between sources of high-energy radiation and GWs. The most luminous high-energy sources—gamma-ray bursts (GRBs)—have long been considered as very likely sources of GWs, particularly from short-duration GRBs, which are thought to originate from the merger of two compact objects such as binary neutron stars and a neutron star–black hole binary. In this paper, we discuss: (i) the high-energy emission from short-duration GRBs; (ii) what other sources of high-energy radiation may be observed from binary mergers; and (iii) how searches for high-energy electromagnetic counterparts to GW events are performed with current space facilities. While current high-energy facilities, such as Swift and Fermi, play a crucial role in the search for electromagnetic counterparts, new space missions will greatly enhance our capabilities for joint observations. We discuss why such facilities, which incorporate new technology that enables very wide-field X-ray imaging, are required if we are to truly exploit the multi-messenger era. This article is part of a discussion meeting issue ‘The promises of gravitational-wave astronomy’.

VEGA, AN ENVIRONMENT FOR GRAVITATIONAL WAVES DATA ANALYSIS

2000 ◽  
Vol 09 (03) ◽  
pp. 293-297 ◽  
Author(s):  
D. BUSKULIC ◽  
L. DEROME ◽  
R. FLAMINIO ◽  
F. MARION ◽  
L. MASSONET ◽  
...  
Keyword(s):  
Data Analysis ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Large Scale ◽  
Data Access ◽  
The World ◽  
Gravitational Wave Detectors ◽  
Batch Data ◽  
New Generation

A new generation of large scale and complex Gravitational Wave detectors is building up. They will produce big amount of data and will require intensive and specific interactive/batch data analysis. We will present VEGA, a framework for such data analysis, based on ROOT. VEGA uses the Frame format defined as standard by GW groups around the world. Furthermore, new tools are developed in order to facilitate data access and manipulation, as well as interface with existing algorithms. VEGA is currently evaluated by the VIRGO experiment.

NEW ASPECTS ON GRAVITATIONAL WAVE EMISSION BY NEUTRON STARS

2004 ◽  
Vol 13 (07) ◽  
pp. 1293-1296 ◽  
Author(s):  
GUILHERME F. MARRANGHELLO ◽  
CÉSAR A. Z. VASCONCELLOS ◽  
JOSÉ A. de FREITAS PACHECO ◽  
MANFRED DILLIG ◽  
HÉLIO T. COELHO
Keyword(s):  
Phase Transition ◽  
Equation Of State ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Quark Matter ◽  
Inner Core ◽  
Compact Objects ◽  
Wave Emission

We discuss, in this work, new aspects related to the emission of gravitational waves by neutron stars, which undergo a phase transition, from nuclear to quark matter, in its inner core. Such a phase transition would liberate around 1052–53 erg of energy in the form of gravitational waves which, if detected, may shed some light in the structure of these compact objects and provide new insights on the equation of state of nuclear matter.

scholarly journals ELECTROMAGNETIC COUNTERPARTS OF GRAVITATIONAL WAVE SOURCES: MERGERS OF COMPACT OBJECTS

2013 ◽  
Vol 22 (01) ◽  
pp. 1341011 ◽  
Author(s):  
ATISH KAMBLE ◽  
DAVID L. A. KAPLAN
Keyword(s):  
Gravitational Wave ◽  
Gravitational Waves ◽  
Compact Objects ◽  
Detection Rates ◽  
Radio Transients ◽  
The Masses ◽  
Multi Band

Mergers of compact objects are considered prime sources of gravitational waves (GW) and will soon be targets of GW observatories such as the Advanced-LIGO and VIRGO. Finding electromagnetic counterparts of these GW sources will be important to understand their nature. We discuss possible electromagnetic signatures of the mergers. We show that the BH–BH mergers could have luminosities which exceed Eddington luminosity from unity to several orders of magnitude depending on the masses of the merging BHs. As a result these mergers could be explosive, release up to 1051 erg of energy and shine as radio transients. At any given time we expect about a few such transients in the sky at GHz frequencies, which could be detected to be about 300 Mpc. It has also been argued that these radio transients would look alike radio supernovae with comparable detection rates. Multi-band follow-up could, however, distinguish between the mergers and supernovae.

scholarly journals Method of Gravitational Wave Search Based on Adaptive Time-Frequency Analysis and Machine Learning

Impact ◽  
2020 ◽  
Vol 2020 (5) ◽  
pp. 43-45
Author(s):  
Hirotaka Takahashi
Keyword(s):  
Gravitational Wave ◽  
Gravitational Waves ◽  
Large Scale ◽  
Albert Einstein ◽  
Cosmic Ray ◽  
Time Frequency ◽  
Adaptive Time ◽  
Physics Experiment ◽  
The University ◽  
First Time

In simple terms, gravitational waves are ripples in space-time caused by energetic processes in the Universe, such as the movement of mass. One of the exciting things about them is that they can be used to observe systems that are basically impossible to detect using other means. These ripples were predicted by Albert Einstein almost a century ago, but it wasn't until 2016 that scientists announced, for the first time, the detection of gravitational waves. The Laser Interferometer Gravitational-Wave Observatory (LIGO) is the physics experiment responsible for this detection and it has since continued to make a significant impact in the field. LIGO collaborates closely with the Virgo interferometer; a large interferometer designed to detect gravitational waves, and the Japanese Gravitational Wave Detector in Kamioka Mine (KAGRA), the Large Scale Cryogenic Gravitational Wave Telescope; a project of the gravitational wave studies group led by the Institute for Cosmic Ray Research of The University of Tokyo. But there still remain many unknowns, such as challenges related to the data analysis of gravitational waves. Professor Hirotaka Takahashi is carrying out research on gravitational waves that is attempting to address these challenges by developing algorithms that can dramatically increase the speed and efficiency of gravitational wave searches, which he believes are currently insufficient. Takahashi is a member of the KAGRA collaboration, which, as of March 2020, consists of more than 390 researchers from 90 institutions in 14 countries and regions.

scholarly journals On Dark Gravitational Wave Standard Sirens as Cosmological Inference and Forecasting the Constraint on Hubble Constant using Binary Black Holes Detected by Deci-Hertz Observator

2021 ◽  
Author(s):  
Ju Chen ◽  
Changshuo Yan ◽  
Youjun Lu ◽  
Yuetong Zhao ◽  
Junqiang Ge
Keyword(s):  
Black Holes ◽  
Gravitational Wave ◽  
Signal To Noise Ratio ◽  
Cosmological Parameters ◽  
Hubble Constant ◽  
Luminosity Distance ◽  
Host Galaxies ◽  
Binary Black Holes ◽  
Merger Rate ◽  
Electromagnetic Signals

Abstract Gravitational wave (GW) signals from compact binary coalescences can be used as standard sirens to constrain cosmological parameters if its redshift can be measured independently by electromagnetic signals. However, mergers of stellar binary black holes (BBHs) may not have electromagnetic counterparts and thus have no direct redshift measurements. These dark sirens may be still used to statistically constrain cosmological parameters by combining their GW measured luminosity distances and localization with deep redshift surveys of galaxies around it. We investigate this dark siren method to constrain cosmological parameters in details by using mock BBH and galaxy samples. We find that the Hubble constant can be well constrained with an accuracy $\lesssim 1\%$ with a few tens or more BBH mergers at redshift up to $1$ if GW observations can provide accurate estimates of its luminosity distance (with relative error of $\lesssim 0.01$) and localization ($\lesssim 0.1\mathrm{deg}^2$), though the constraint may be significantly biased if the luminosity distance and localization errors are larger. We further generate mock BBH samples, according to current constraints on BBH merger rate and the distributions of BBH properties, and find that Deci-Hertz Observatory (DO) in a half year observation period may detect about one hundred BBHs with signal-to-noise ratio $\varrho \gtrsim 30$, relative luminosity distance error $\lesssim 0.02$, and localization error $\lesssim 0.01\mathrm{deg}^2$. By applying the dark standard siren method, we find that the Hubble constant can be constrained to $\sim 0.1-1\%$ level using these DO BBHs, an accuracy comparable to the constraints obtained by using electromagnetic observations in the near future, thus it may provide insight into the Hubble tension. We also demonstrate that the constraint on the Hubble constant using this dark siren method are robust and do not depend on the choice of the prior for the properties of BBH host galaxies.

scholarly journals Gravitational-Wave Implications for the Parity Symmetry of Gravity at GeV Scale

2020 ◽  
Author(s):  
Yifan Wang ◽  
Rui Niu ◽  
Wen Zhao ◽  
Tao Zhu
Keyword(s):  
General Relativity ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Particle Physics ◽  
Energy Region ◽  
High Energy ◽  
Energy Scale ◽  
High Energy Region ◽  
Parity Symmetry ◽  
Parity Conservation

Abstract Einstein's general relativity, as the most successful theory of gravity, is one of the cornerstones of modern physics. However, the experimental tests for gravity in the high energy region are limited. The emerging gravitational-wave astronomy has opened an avenue for probing the fundamental properties of gravity in strong and dynamical field, and in particular, high energy regime. In this work, we focus on the parity symmetry of gravity. For broken parity, the left- and right-handed modes of gravitational waves would follow different equations of motion, dubbed as birefringence. We perform the first full Bayesian inference of the parity conservation of gravity by comparing the state-of-the-art waveform with the compact binary coalescence data released by LIGO and Virgo collaboration. We do not find any violations of general relativity, thus obtain the lower bound of the parity-violating energy scale to be $0.09$ GeV through the velocity birefringence of gravitational waves. This provides the most stringent experimental test of gravitational parity symmetry up to date, and for the first time, in the high energy region, which ushers in a new era of using gravitational waves to test the ultraviolet behavior of gravity. We also find third-generation gravitational-wave detectors can enhance this bound to $\mathcal{O}(10^2)$ GeV if there is still no violation, comparable to the current LHC energy scale in particle physics.

JOINT SEARCHES BETWEEN GRAVITATIONAL-WAVE INTERFEROMETERS AND HIGH-ENERGY NEUTRINO TELESCOPES: SCIENCE REACH AND ANALYSIS STRATEGIES

2009 ◽  
Vol 18 (10) ◽  
pp. 1655-1659 ◽  
Author(s):  
VERONIQUE VAN ELEWYCK ◽  
S. ANDO ◽  
Y. ASO ◽  
B. BARET ◽  
M. BARSUGLIA ◽  
...  
Keyword(s):  
Gravitational Wave ◽  
Gravitational Waves ◽  
High Energy ◽  
Directional Information ◽  
High Energy Neutrino ◽  
Neutrino Telescopes ◽  
Energy Neutrino ◽  
Analysis Strategies ◽  
High Energy Neutrinos

Many of the astrophysical sources and violent phenomena observed in our Universe are potential emitters of gravitational waves (GWs) and high-energy neutrinos (HENs). A network of GW detectors such as LIGO and Virgo can determine the direction/time of GW bursts while the IceCube and ANTARES neutrino telescopes can also provide accurate directional information for HEN events. Requiring the consistency between both, totally independent, detection channels shall enable new searches for cosmic events arriving from potential common sources, of which many extra-galactic objects.

scholarly journals Gravitational waves from in-spirals of compact objects in binary common-envelope evolution

2020 ◽  
Vol 493 (4) ◽  
pp. 4861-4867 ◽  
Author(s):  
Yonadav Barry Ginat ◽  
Hila Glanz ◽  
Hagai B Perets ◽  
Evgeni Grishin ◽  
Vincent Desjacques
Keyword(s):  
Gravitational Wave ◽  
Gravitational Waves ◽  
Compact Objects ◽  
Dynamical Friction ◽  
Next Generation ◽  
Common Envelope ◽  
Dissipative Processes

ABSTRACT Detection of gravitational-wave (GW) sources enables the characterization of binary compact objects (COs) and of their in-spiral. However, other dissipative processes can affect the in-spiral. Here, we show that the in-spiral of COs through a gaseous common envelope (CE) arising from an evolved stellar companion produces a novel type of GW sources, whose evolution is dominated by the dissipative gas dynamical friction effects from the CE, rather than the GW emission itself. The evolution and properties of the GW signals differ from those of isolated gas-poor mergers significantly. We find characteristic strains of ∼10−23–10−21 ($10\, {\rm kpc}/{D}$) for such sources – observable by next-generation space-based GW detectors (at rates of once per a few centuries for LISA, and about once a year for BBO). The evolution of the GW signal can serve as a probe of the interior regions of the evolved star, and the final stages of CE evolution, otherwise inaccessible through other observational means. Moreover, such CE mergers are frequently followed by observable explosive electromagnetic counterparts and/or the formation of exotic stars.

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