作者: 放縱 時間: 2025-3-21 21:36
https://doi.org/10.1007/978-3-476-02811-2f the expected GW signal, highlighting its dependence on the overall binary population, the relation between SMBHs and their hosts, and their coupling with the stellar and gaseous environment. I describe the status of current PTA efforts, and prospect of future detection and SMBH binary astrophysics.作者: nonchalance 時間: 2025-3-22 04:03 作者: Dri727 時間: 2025-3-22 06:46 作者: encomiast 時間: 2025-3-22 10:30
The Coalescence Rates of Compact Object Binaries,ulations of binary evolution. The two methods give consistent results, yet the uncertainties are still quite large. Nevertheless the current estimates point that the probability of detection of gravitational waves in the coming years is quite high.作者: 憤慨一下 時間: 2025-3-22 14:02 作者: 憤慨一下 時間: 2025-3-22 20:30 作者: 預測 時間: 2025-3-23 01:10 作者: 復習 時間: 2025-3-23 02:40
Biofeedback in der Narbentherapie,stant specific angular momentum profile that we study, we observe a significant change of the disk shape after a few orbits. This change is more pronounced the larger the initial inclination angle is.作者: forebear 時間: 2025-3-23 07:50 作者: PALL 時間: 2025-3-23 20:58 作者: 錯事 時間: 2025-3-23 23:57
Interpersonal and Social Dynamics,e present preliminary results from a class of tidal disruption events that until now have not been considered in which the disruption-flare-disk sequence develops promptly. These tidal disruption events are from ultra-close encounters between main-sequence stars and intermediate mass black holes.作者: 藝術 時間: 2025-3-24 03:23
Yves Dauvilliers,Giuseppe Plazziion of supermassive black holes from their host galaxies. We also discuss possible mechanisms that would make superkicks less likely to occur in astrophysical binaries and thus explain why most, if not all, galaxies observed in this context appear to harbor a black hole at their center.作者: Mere僅僅 時間: 2025-3-24 09:42 作者: 入會 時間: 2025-3-24 12:10 作者: 華而不實 時間: 2025-3-24 18:55
Gravitational Recoil and Astrophysical Impact,ion of supermassive black holes from their host galaxies. We also discuss possible mechanisms that would make superkicks less likely to occur in astrophysical binaries and thus explain why most, if not all, galaxies observed in this context appear to harbor a black hole at their center.作者: 你敢命令 時間: 2025-3-24 22:27 作者: Ganglion-Cyst 時間: 2025-3-25 01:33
https://doi.org/10.1007/978-1-4684-1869-9he parametric, turbulent instability of scalar fields on a background which includes a gravitational QNM, and the shifts to the QNM frequencies of Kerr when the black hole is weakly charged. This method may be of use in studies of black holes which are deformed by external fields or are solutions to alternative theories of gravity.作者: 劇本 時間: 2025-3-25 06:24 作者: 蜈蚣 時間: 2025-3-25 10:21 作者: spinal-stenosis 時間: 2025-3-25 14:15 作者: FAWN 時間: 2025-3-25 17:16 作者: 注意 時間: 2025-3-25 20:17
Localizing Gravitational Wave Sources with Optical Telescopes and Combining Electromagnetic and Graalso potential electromagnetic (EM) emitters. Gravitational waves will provide a new window to observe these events and hopefully give us glimpses of new astrophysics. In this paper, we discuss how EM information of these events can considerably improve GW parameter estimation both in terms of accur作者: CAMP 時間: 2025-3-26 01:55 作者: 貴族 時間: 2025-3-26 05:07 作者: MOAN 時間: 2025-3-26 09:04
Gravitational Waves from Rapidly Rotating Neutron Stars,nt estimates of the gravitational wave emission for various scenarios, given the (electromagnetically) observed characteristics of these systems. First of all we focus on the r-mode instability and show that a “minimal” neutron star model (which does not incorporate exotica in the core, dynamically 作者: engrossed 時間: 2025-3-26 15:39 作者: Myofibrils 時間: 2025-3-26 18:17 作者: Melatonin 時間: 2025-3-26 22:02 作者: cavity 時間: 2025-3-27 03:01
Rival Families: Waveforms from Resonant Black-Hole Binaries as Probes of Their Astrophysical Formatewtonian theory predicts the existence of two one-parameter families of equilibrium solutions (“resonances”) in which the angular momentum and both spins share a common plane and precess at the same frequency. The two families are differentiated by either aligned or anti-aligned spin components in t作者: 費解 時間: 2025-3-27 09:04 作者: Chivalrous 時間: 2025-3-27 09:37
Gravitational Wave Verification Sources, weak gravitational wave sources. However, there are nine systems where the gravitational wave strain is strong enough to make them verification sources for gravitational wave missions, e.g. the evolved Laser Interferometer Space Antenna (.). Here we present a summary of the physical characteristics作者: MEAN 時間: 2025-3-27 16:43
The Gravitational Wave Emission of White Dwarf Dynamical Interactions, it with the sensitivity curves of planned space-borne gravitational wave detectors, like eLISA and ALIA. We find that for the three possible outcomes of these interactions—which are the formation of an eccentric binary system, a lateral collision in which several mass transfer episodes occur, and a作者: 令人不快 時間: 2025-3-27 20:54
Gravitational Recoil and Astrophysical Impact,tion, imparts a gravitational recoil on the emitting source. Numerical relativity simulations have revealed that this effect can lead to astonishingly large kick velocities, so-called ., of several thousand km/s in the inspiral and merger of black-hole binaries. We here discuss the calculation of th作者: engrossed 時間: 2025-3-28 01:15 作者: 分散 時間: 2025-3-28 03:49
Extraction of GWs from a Numerical Simulation,d characteristic extraction. These methods are reviewed, and the strengths and weaknesses of each method are discussed. The accuracy of the methods is compared for astrophysical scenarios that are commonly simulated numerically.作者: 問到了燒瓶 時間: 2025-3-28 08:39
Quasinormal Modes Beyond Kerr,rr black holes. We discuss a method for computing the QNMs of spacetimes which are slightly deformed from Kerr. We mention two example applications: the parametric, turbulent instability of scalar fields on a background which includes a gravitational QNM, and the shifts to the QNM frequencies of Ker作者: 圣人 時間: 2025-3-28 10:59
https://doi.org/10.1007/978-0-387-28745-4Currently, the best experiments supporting this hypothesis are based on high-precision timing of radio pulsars. This chapter reviews recent advances in the field with a focus on compact binary millisecond pulsars with white-dwarf (WD) companions. These systems—if modeled properly—provide an unparall作者: 暗諷 時間: 2025-3-28 18:39
Nantgarw and Swansea PorcelainsInvestigating their properties was hampered by their elusive nature: only a handful are known. In this paper I review the estimates of the compact object merger rate density. This rate density can be estimated based directly on observations of objects that will merge, or using elaborate computer sim作者: 安裝 時間: 2025-3-28 20:45
https://doi.org/10.1007/978-3-476-01496-2 of a vast range of astronomical phenomena. Uncertainties in the source sky location estimate from gravitational wave observations mean follow-up observatories must scan large portions of the sky for a potential companion signal. A general frame of joint GW-EM observations is presented by a multi-me作者: Innocence 時間: 2025-3-29 00:42
Opposition: the Politics of Nostalgia,y burst (GRB), GRB 090227B, allow to give an estimate of the gravitational waves versus the X and gamma-rays emission in a short GRB. NS binaries represent good candidates for the detection of gravitational waves emitted during the spiraling-in and final merging phase of the system that leads to the作者: 大吃大喝 時間: 2025-3-29 06:31 作者: 不法行為 時間: 2025-3-29 10:43 作者: 騎師 時間: 2025-3-29 13:19
Kleist als Dichter des Widerstands,Indeed, if the black-hole which forms after the merger, is surrounded by a massive disk, neutrino annihilation processes may produce high-energy and collimated electromagnetic radiation. In this paper, we devise a new procedure, to be used in the search for gravitational waves from black-hole-neutro作者: Confound 時間: 2025-3-29 16:32
https://doi.org/10.1007/978-3-662-68482-5nt estimates of the gravitational wave emission for various scenarios, given the (electromagnetically) observed characteristics of these systems. First of all we focus on the r-mode instability and show that a “minimal” neutron star model (which does not incorporate exotica in the core, dynamically 作者: 樹上結蜜糖 時間: 2025-3-29 21:47
Biofeedback in der Narbentherapie,tructure in the universe. They however remain observationally elusive, thus raising a question about characteristic observational signatures associated with these systems. In this conference proceeding I discuss current theoretical understanding and latest advances and prospects in observational sea作者: Terrace 時間: 2025-3-30 03:09
Biofeedback in der Narbentherapie,ploy the EinsteinToolkit, using the thorn McLachlan for the evolution of the spacetime via the BSSN formalism of the Einstein equations and the thorn GRHydro for the evolution of the hydrodynamics, using a 3D Cartesian mesh with adaptive mesh refinement. We investigate the effects of the tilt angle 作者: Ornament 時間: 2025-3-30 04:48 作者: 索賠 時間: 2025-3-30 09:25
https://doi.org/10.1007/978-3-319-60330-8ewtonian theory predicts the existence of two one-parameter families of equilibrium solutions (“resonances”) in which the angular momentum and both spins share a common plane and precess at the same frequency. The two families are differentiated by either aligned or anti-aligned spin components in t作者: Custodian 時間: 2025-3-30 15:00
https://doi.org/10.1007/978-3-476-02811-2ition of all waves emitted by the cosmological population of supermassive black hole (SMBH) binaries. Such superposition creates an incoherent stochastic background, on top of which particularly bright or nearby sources might be individually resolved. In this contribution I describe the properties o作者: Prostaglandins 時間: 2025-3-30 16:37
,Postscript: From Culiacán to Cannes, weak gravitational wave sources. However, there are nine systems where the gravitational wave strain is strong enough to make them verification sources for gravitational wave missions, e.g. the evolved Laser Interferometer Space Antenna (.). Here we present a summary of the physical characteristics作者: Glossy 時間: 2025-3-30 23:31
https://doi.org/10.1007/978-3-319-23739-8 it with the sensitivity curves of planned space-borne gravitational wave detectors, like eLISA and ALIA. We find that for the three possible outcomes of these interactions—which are the formation of an eccentric binary system, a lateral collision in which several mass transfer episodes occur, and a作者: LOPE 時間: 2025-3-31 01:28
Yves Dauvilliers,Giuseppe Plazzition, imparts a gravitational recoil on the emitting source. Numerical relativity simulations have revealed that this effect can lead to astonishingly large kick velocities, so-called ., of several thousand km/s in the inspiral and merger of black-hole binaries. We here discuss the calculation of th作者: MURKY 時間: 2025-3-31 08:43
Mathematical Models of Narcolepsyte as fCCZ4, well suited for curvilinear as well as Cartesian coordinates. We implement this formalism in spherical polar coordinates under the assumption of spherical symmetry using a partially-implicit Runge-Kutta (PIRK) method, without using any regularization scheme, and show that our code can e作者: 法律的瑕疵 時間: 2025-3-31 10:55 作者: Glutinous 時間: 2025-3-31 14:38
https://doi.org/10.1007/978-1-4684-1869-9rr black holes. We discuss a method for computing the QNMs of spacetimes which are slightly deformed from Kerr. We mention two example applications: the parametric, turbulent instability of scalar fields on a background which includes a gravitational QNM, and the shifts to the QNM frequencies of Ker作者: 違法事實 時間: 2025-3-31 19:18 作者: CANDY 時間: 2025-4-1 01:39 作者: CAB 時間: 2025-4-1 03:57
Prologue Napoleon and the French Revolution,e show some preliminary results in the context of an array of optical telescopes called BlackGEM, dedicated for optical follow-up of GW triggers, that is being constructed in La Silla, Chile and is expected to operate concurrent to the advanced GW detectors.作者: Wordlist 時間: 2025-4-1 08:52 作者: 高歌 時間: 2025-4-1 13:03
Kleist als Dichter des Widerstands,e used in low-latency data analysis to restrict the parameter space searching for gravitational signals associated with short gamma-ray bursts, and to gain information on the dynamics of the coalescing system and on the neutron star equation of state.作者: Biofeedback 時間: 2025-4-1 15:21 作者: evanescent 時間: 2025-4-1 19:12
https://doi.org/10.1007/978-3-319-60330-8oise ratios?～?10, typical of those expected for the first detections with Advanced LIGO/Virgo. Spin-orbit resonances thus consist in powerful, viable, probes of astrophysical processes in stellar-mass black-hole binary formation and evolution.作者: NEX 時間: 2025-4-2 01:00 作者: 者變 時間: 2025-4-2 04:19
X, Gamma-Rays, and Gravitational Waves Emission in a Short Gamma-Ray Burst,?2?Gpc. We assess the detectability of this source by the Advanced LIGO interferometer computing the signal-to-noise ratio (SNR) averaged over all polarizations and possible positions of the source with respect to the interferometer. We simulate the dynamics of the binary up to the contact point usi作者: FEAS 時間: 2025-4-2 09:05
Localizing Gravitational Wave Sources with Optical Telescopes and Combining Electromagnetic and Grae show some preliminary results in the context of an array of optical telescopes called BlackGEM, dedicated for optical follow-up of GW triggers, that is being constructed in La Silla, Chile and is expected to operate concurrent to the advanced GW detectors.
