scholarly journals Gravitational wave signatures of the absence of an event horizon. II. Extreme mass ratio inspirals in the spacetime of a thin-shell gravastar

2010 ◽  
Vol 81 (8) ◽  
Author(s):  
Paolo Pani ◽  
Emanuele Berti ◽  
Vitor Cardoso ◽  
Yanbei Chen ◽  
Richard Norte
Keyword(s):  
Gravitational Wave ◽  
Event Horizon ◽  
Thin Shell ◽  
Mass Ratio

scholarly journals Gravitational wave signatures of the absence of an event horizon: Nonradial oscillations of a thin-shell gravastar

2009 ◽  
Vol 80 (12) ◽  
Author(s):  
Paolo Pani ◽  
Emanuele Berti ◽  
Vitor Cardoso ◽  
Yanbei Chen ◽  
Richard Norte
Keyword(s):  
Gravitational Wave ◽  
Event Horizon ◽  
Thin Shell ◽  
Nonradial Oscillations

scholarly journals Gravitational Wave Glitches in Chaotic Extreme-Mass-Ratio Inspirals

2021 ◽  
Vol 126 (14) ◽  
Author(s):  
Kyriakos Destounis ◽  
Arthur G. Suvorov ◽  
Kostas D. Kokkotas
Keyword(s):  
Gravitational Wave ◽  
Mass Ratio

scholarly journals Isotropic Gravastar Model in Rastall Gravity

2020 ◽  
Vol 2020 ◽  
pp. 1-10
Author(s):  
G. Abbas ◽  
K. Majeed
Keyword(s):  
Black Hole ◽  
Event Horizon ◽  
Analytical Solutions ◽  
Thin Shell ◽  
Graphical Analysis ◽  
Stiff Fluid ◽  
Matter Distribution ◽  
The Third ◽  
Schwarzschild Geometry ◽  
Third Phase

In the present paper, we have introduced a new model of gravastar with an isotropic matter distribution in Rastall gravity by the Mazur–Mottola (2004) mechanism. Mazur–Mottola approach is about the construction of gravastar which is predicted as an alternative to black hole. By following this convention, we define gravastar in the form of three phases. The first one is an interior phase which has negative density; the second part consists of thin shell comprising ultrarelativistic stiff fluid for which we have discussed the length, energy, and entropy. By the graphical analysis of entropy, we have shown that our proposed thin shell gravastar model is potentially stable. The third phase of gravastar is defined by the exterior Schwarzschild geometry. For the interior of gravastar, we have found the analytical solutions free from any singularity and the event horizon in the framework of Rastall gravity.

scholarly journals The gravitational wave 'probability event horizon' for double neutron star mergers

2005 ◽  
Vol 364 (3) ◽  
pp. 807-812 ◽  
Author(s):  
D. M. Coward ◽  
M. Lilley ◽  
E. J. Howell ◽  
R. R. Burman ◽  
D. G. Blair
Keyword(s):  
Neutron Star ◽  
Gravitational Wave ◽  
Event Horizon

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 Gravitational wave astronomy, relativity tests, and massive black holes

2009 ◽  
Vol 5 (S261) ◽  
pp. 240-248 ◽  
Author(s):  
Peter L. Bender
Keyword(s):  
General Relativity ◽  
Gravitational Wave ◽  
Galactic Center ◽  
Galactic Nuclei ◽  
Compact Objects ◽  
Mass Ratio ◽  
Intermediate Mass ◽  
Massive Black Holes ◽  
New Information ◽  
Laser Interferometer Space Antenna

AbstractThe gravitational wave detectors that are operating now are looking for several kinds of gravitational wave signals at frequencies of tens of Hertz to kilohertz. One of these is mergers of roughly 10 M⊙ BH binaries. Sometime between now and about 8 years from now, it is likely that signals of this kind will be observed. The result will be strong tests of the dynamical predictions of general relativity in the high field regime. However, observations at frequencies below 1 Hz will have to wait until the launch of the Laser Interferometer Space Antenna (LISA), hopefully only a few years later. LISA will have 3 main objectives, all involving massive BHs. The first is observations of mergers of pairs of intermediate mass (100 to 105M⊙) and higher mass BHs at redshifts out to roughly z=10. This will provide new information on the initial formation and growth of BHs such as those found in most galaxies, and the relation between BH growth and the evolution of galactic structure. The second objective is observations of roughly 10 M⊙ BHs, neutron stars, and white dwarfs spiraling into much more massive BHs in galactic nuclei. Such events will provide detailed information on the populations of such compact objects in the regions around galactic centers. And the third objective is the use of the first two types of observations for testing general relativity even more strongly than ground based detectors will. As an example, an extreme mass ratio event such as a 10 M⊙ BH spiraling into a galactic center BH can give roughly 105 observable cycles during about the last year before merger, with a mean relative velocity of 1/3 to 1/2 the speed of light, and the frequencies of periapsis precession and Lense-Thirring precession will be high. The LISA Pathfinder mission to prepare for LISA is scheduled for launch in 2011.

scholarly journals Gravitational wave detection in space

2016 ◽  
Vol 25 (14) ◽  
pp. 1630001 ◽  
Author(s):  
Wei-Tou Ni
Keyword(s):  
Black Holes ◽  
Gravitational Wave ◽  
Frequency Band ◽  
Low Frequency ◽  
Big Bang ◽  
Mass Ratio ◽  
Intermediate Mass ◽  
Compact Binaries ◽  
Laser Interferometer Space Antenna ◽  
Deployment Time

Gravitational Wave (GW) detection in space is aimed at low frequency band (100[Formula: see text]nHz–100[Formula: see text]mHz) and middle frequency band (100[Formula: see text]mHz–10[Formula: see text]Hz). The science goals are the detection of GWs from (i) Supermassive Black Holes; (ii) Extreme-Mass-Ratio Black Hole Inspirals; (iii) Intermediate-Mass Black Holes; (iv) Galactic Compact Binaries and (v) Relic GW Background. In this paper, we present an overview on the sensitivity, orbit design, basic orbit configuration, angular resolution, orbit optimization, deployment, time-delay interferometry (TDI) and payload concept of the current proposed GW detectors in space under study. The detector proposals under study have arm length ranging from 1000[Formula: see text]km to [Formula: see text][Formula: see text]km (8.6[Formula: see text]AU) including (a) Solar orbiting detectors — (ASTROD Astrodynamical Space Test of Relativity using Optical Devices (ASTROD-GW) optimized for GW detection), Big Bang Observer (BBO), DECi-hertz Interferometer GW Observatory (DECIGO), evolved LISA (e-LISA), Laser Interferometer Space Antenna (LISA), other LISA-type detectors such as ALIA, TAIJI etc. (in Earthlike solar orbits), and Super-ASTROD (in Jupiterlike solar orbits); and (b) Earth orbiting detectors — ASTROD-EM/LAGRANGE, GADFLI/GEOGRAWI/g-LISA, OMEGA and TIANQIN.

scholarly journals Gravitational-wave signature of a thin-shell gravastar

2010 ◽  
Vol 222 ◽  
pp. 012032 ◽  
Author(s):  
Paolo Pani ◽  
Emanuele Berti ◽  
Vitor Cardoso ◽  
Yanbei Chen ◽  
Richard Norte
Keyword(s):  
Gravitational Wave ◽  
Thin Shell ◽  
Wave Signature
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