Black (W)hole: An Artscience and Education Collaboration

Leonardo ◽  
2016 ◽  
Vol 49 (1) ◽  
pp. 19-24 ◽  
Author(s):  
Sara Mast ◽  
Jessica Jellison ◽  
Christopher O’Leary ◽  
Jason Bolte ◽  
Cindy Stillwell ◽  
...  
Keyword(s):  
Black Hole ◽  
Science Education ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Data Visualization ◽  
21St Century ◽  
Mass Ratio ◽  
Art Installation ◽  
Mind And Body ◽  
Astronomical Object

Black (W)hole is an immersive art installation created collaboratively by artists and scientists utilizing data visualization of an extreme mass ratio inspiral (EMRI) and the sonification of its emitted gravitational waves in an experiential work of “artscience” and science education. The sensory-rich environment of the installation engages mind and body, expanding and enriching the participant’s capacity to imagine and wonder about the beauty and meaning of this highly abstract astronomical object, the black hole. The work investigates both historical and current gravitational wave astronomy, illustrating our 21st-century understanding of the cosmos.

scholarly journals The Taiji program: A concise overview

2020 ◽  
Author(s):  
Ziren Luo ◽  
Yan Wang ◽  
Yueliang Wu ◽  
Wenrui Hu ◽  
Gang Jin
Keyword(s):  
Black Hole ◽  
Gravitational Waves ◽  
Frequency Band ◽  
Space Mission ◽  
Mass Ratio ◽  
Intermediate Mass ◽  
Concise Overview

Abstract Taiji is a Chinese space mission to detect gravitational waves in the frequency band 0.1 mHz to 1.0 Hz, which aims at detecting super (intermediate) mass black hole mergers and extreme (intermediate) mass ratio in-spirals. A brief introduction of its mission overview, scientific objectives, and payload design is presented. A roadmap is also given in which the launching time is set to the 2030s.

Electromagnetic counterpart to gravitational waves from coalescence of binary black hole with magnetic monopole charge

2020 ◽  
Vol 35 (31) ◽  
pp. 2050205
Author(s):  
Aung Naing Win ◽  
Yu-Ming Chu ◽  
Hasrat Hussain Shah ◽  
Syed Zaheer Abbas ◽  
Munawar Shah
Keyword(s):  
Black Hole ◽  
Dipole Moment ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Short Duration ◽  
Electric Dipole Moment ◽  
Electric Dipole ◽  
Magnetic Monopole ◽  
Compact Object ◽  
Binary Black Hole

A Satellite Fermi GBM detected recent putative short Gamma Ray Bursts (GRBs) in coincident with the gravitational wave signal GW 150914 produced by the merger of binary black hole (BH). If at least one BH possess magnetic monopole charge in the binary BH system then the short-duration GRBs may produce during the final phase of a binary BH merger. The detection of gravitational waves GW 150914, GW 151226 and LVT 151012 by LIGO gave the evidence that merging of the compact object like binary BH often happens in our universe. In this paper, we report the qualitative model to discuss the generation of electromagnetic radiation from the merging of two BHs with equal masses and at least one BH carrying the magnetic monopole charge in the binary system. In this model, BH possess a magnetic monopole charge that may not be neutralized before the coalescence. During the inspiralling process, the magnetic monopole charge on the BH would produced the electric dipole moment. Short duration GRB would produce by the rapidly evolution of the electric dipole moment which may detectable on Earth. We predict that this model would be beneficial in the future to explain the generation of gravitational wave (GW) plus a electromagnetic signal of multi-wavelength from mergers of magnetically charged BHs.

scholarly journals BLACK HOLES COLLISION IN GENERAL ROBINSON-TRAUTMAN SPACETIMES: WAVE FORMS AND THE EFFICIENCY OF THE GRAVITATIONAL WAVE EXTRACTION

2011 ◽  
Vol 03 ◽  
pp. 408-416
Author(s):  
H. P. DE OLIVEIRA ◽  
E. L. RODRIGUES
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Spectral Methods ◽  
Numerical Code ◽  
Numerical Evidence ◽  
Nonextensive Statistics ◽  
Wave Forms ◽  
Frontal Collisions

We analyze the non-frontal collisions of two Schwarzschild black holes in the realm of general Robinson-Trautman spacetimes using a numerical code based on spectral methods. In this process, two black holes collide and form a single black hole while a certain amount of the initial mass is carried away by gravitational waves. We determined the forms of the gravitational waves and the efficiency of this process for frontal and non-frontal collisions. We found numerical evidence that the distribution of mass qloss can be described by a function typically used in nonextensive statistics.

The development of ground based gravitational wave astronomy and opportunities for Australia–China collaboration

2015 ◽  
Vol 30 (28n29) ◽  
pp. 1545019
Author(s):  
David Blair ◽  
Li Ju ◽  
Chunnong Zhao ◽  
Linqing Wen ◽  
Qi Chu ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Southern Hemisphere ◽  
Event Rate ◽  
Wave Spectrum ◽  
Current Status ◽  
Dramatic Improvement ◽  
The Universe

This paper begins by reviewing the development of gravitational wave astronomy from the first predictions of gravitational waves to development of technologies across the entire gravitational wave spectrum, and then focuses on the current status of ground based gravitational wave detectors. With substantial improvements already demonstrated in early commissioning it is emphasised that Advanced detectors are on track for first detection of gravitational waves. The importance of a worldwide array of detectors is emphasised, and recent results are shown that demonstrate the continued advantage of a southern hemisphere detector. Finally it is shown that a north–south pair of 8 km arm length detectors would give rise to a dramatic improvement in event rate, enabling a pair of detectors to encompass a 64-times larger volume of the universe, to conduct a census on all stellar mass black hole mergers to [Formula: see text] and to observe neutron star mergers to a distance of [Formula: see text][Formula: see text]800 Mpc.

scholarly journals Testing Gravity Theory With Extreme Mass-Ratio Inspirals: Recent Progress

Proceedings ◽  
2019 ◽  
Vol 17 (1) ◽  
pp. 11
Author(s):  
Shucheng Yang ◽  
Shuo Xin ◽  
Chen Zhang ◽  
Wenbiao Han
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Recent Progress ◽  
Central Body ◽  
Low Frequency ◽  
Kerr Black Hole ◽  
Compact Object ◽  
Wave Dispersion ◽  
Gravity Theory ◽  
Mass Ratio

A compact object captured by a supermassive black hole, named as extreme-mass-ratio inspiral (EMRI), is one of the most important gravitational wave sources for low-frequency interferometers such as LISA, Taiji, and TianQin. EMRIs can be used to accurately map the space-time of the central massive body. In the present paper, we introduce our recent progress on testing gravity theory with EMRIs. We demonstrate how to constrain gravitational wave dispersion and measure the deviation of the central body from the Kerr black hole. By using binary-EMRIs, the gravitational recoil and mass loss due to merger will be measured in a higher accuracy compared with the current LIGO observations. All these potential constrains and measurements will be useful for test of the gravity theory.

scholarly journals Extreme mass-ratio gravitational-wave sources: Mass segregation and post binary tidal-disruption captures

2020 ◽  
Author(s):  
Yael Raveh ◽  
Hagai B Perets
Keyword(s):  
Black Hole ◽  
Gravitational Wave ◽  
Mass Function ◽  
Compact Objects ◽  
Relaxation Processes ◽  
Mass Ratio ◽  
Eccentric Orbits ◽  
Close Proximity ◽  
Nuclear Clusters ◽  
Mass Segregation

Abstract The gravitational-wave (GW) inspirals of stellar-mass compact objects onto a supermassive black hole (MBH), are some of the most promising GW sources detectable by next-generation space-born GW-detectors. The rates and characteristics of such extreme mass ratio inspirals (EMRIs) sources are highly uncertain. They are determined by the dynamics of stars near MBHs, and the rate at which compacts objects are driven to the close proximity of the MBH. Here we consider weakly and strongly mass-segregated nuclear clusters, and the evolution of stars captured into highly eccentric orbits following binary disruptions by the MBH. We make use of a Monte-Carlo approach to model the diffusion of both captured objects, and compact-objects brought through two-body relaxation processes. We calculate the rates of GW-inspirals resulting from relaxation-driven objects, and characterize EMRIs properties. We correct previous studies and show that relaxation-driven sources produce GW-sources with lower-eccentricity than previously found, and provide the detailed EMRI eccentricity distribution in the weak and strong mass-segregation regimes. We also show that binary-disruption captured-stars could introduce low-eccentricity GW-sources of stellar black-hole EMRIs in mass-segregated clusters. The eccentricities of the GW-sources from the capture channel, however, are strongly affected by relaxation processes, and are significantly higher than previously suggested. We find that both the rate and eccentricity distribution of EMRIs could probe the dynamics near MBHs, and the contribution of captured stars, characterize the mass-function of stellar compact objects, and verify whether weak or strong mass-segregation processes take place near MBHs.

scholarly journals Motion deviation of test body induced by spin and cosmological constant in extreme mass ratio inspiral binary system

2019 ◽  
Vol 79 (10) ◽  
Author(s):  
Yu-Peng Zhang ◽  
Shao-Wen Wei ◽  
Pau Amaro-Seoane ◽  
Jie Yang ◽  
Yu-Xiao Liu
Keyword(s):  
Black Hole ◽  
Phase Shift ◽  
Cosmological Constant ◽  
Gravitational Waves ◽  
Test Particle ◽  
Circular Orbit ◽  
Mass Ratio ◽  
Stable Circular Orbit ◽  
Innermost Stable Circular Orbit ◽  
The Impact

Abstract The future space-borne detectors will provide the possibility to detect gravitational waves emitted from extreme mass ratio inspirals of stellar-mass compact objects into supermassive black holes. It is natural to expect that the spin of the compact object and cosmological constant will affect the orbit of the inspiral process and hence lead to the considerable phase shift of the corresponding gravitational waves. In this paper, we investigate the motion of a spinning test particle in the spinning black hole background with a cosmological constant and give the order of motion deviation induced by the particle’s spin and the cosmological constant by considering the corresponding innermost stable circular orbit. By taking the neutron star or kerr black hole as the small body, the deviations of the innermost stable circular orbit parameters induced by the particle’s spin and cosmological constant are given. Our results show that the deviation induced by particle’s spin is much larger than that induced by cosmological constant when the test particle locates not very far away from the black hole, the accumulation of phase shift during the inspiral from the cosmological constant can be ignored when compared to the one induced by the particle’s spin. However when the test particle locates very far away from the black hole, the impact from the cosmological constant will increase dramatically. Therefore the accumulation of phase shift for the whole process of inspiral induced by the cosmological constant and the particle’s spin should be handled with caution.

Sign in / Sign up

Export Citation Format

Share Document