A model for gravitational wave emission from neutrino-driven core-collapse supernovae
TLDR
In this article, a suite of progenitor models, neutrino luminosities, and two-dimensional simulations were used to investigate the matter gravitational wave (GW) emission from postbounce phases of neutrinos-driven core-collapse supernovae.Abstract:
Using a suite of progenitor models, neutrino luminosities, and two-dimensional simulations, we investigate the matter gravitational wave (GW) emission from postbounce phases of neutrino-driven core-collapse supernovae. These phases include prompt and steady-state convection, the standing accretion shock instability (SASI), and asymmetric explosions. For the stages before explosion, we propose a model for the source of GW emission. Downdrafts of the postshock-convection/SASI region strike the protoneutron star "surface" with large speeds and are decelerated by buoyancy forces. We find that the GW amplitude is set by the magnitude of deceleration and, by extension, the downdraft's speed and the vigor of postshock-convective/SASI motions. However, the characteristic frequencies, which evolve from ~100 Hz after bounce to ~300-400 Hz, are practically independent of these speeds (and turnover timescales). Instead, they are set by the deceleration timescale, which is in turn set by the buoyancy frequency at the lower boundary of postshock convection. Consequently, the characteristic GW frequencies are dependent upon a combination of core structure attributes, specifically the dense-matter equation of state (EOS) and details that determine the gradients at the boundary, including the accretion-rate history, the EOS at subnuclear densities, and neutrino transport. During explosion, the high frequency signal wanes and is replaced by a strong low frequency, ~10s of Hz, signal that reveals the general morphology of the explosion (i.e., prolate, oblate, or spherical). However, current and near-future GW detectors are sensitive to GW power at frequencies ≳50 Hz. Therefore, the signature of explosion will be the abrupt reduction of detectable GW emission.read more
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Scheel,Jacob Scheuer,Patricia Schmidt,Patricia Schmidt,Roman Schnabel,R. M. S. Schofield,A. Schönbeck,E. Schreiber,E. Schreiber,B. W. Schulte,B. W. Schulte,Bernard F. Schutz,J. Scott,Susan M. Scott,Edward Seidel,D. Sellers,A. S. Sengupta,N. Sennett,D. Sentenac,V. Sequino,A. Sergeev,Y. Setyawati,Y. Setyawati,Daniel A. Shaddock,T. Shaffer,M. S. Shahriar,M. B. Shaner,Aseem Sharma,Podila Satya Venkata Narasimha Sharma,P. Shawhan,Hongyu Shen,R. Shink,D. H. Shoemaker,D. M. Shoemaker,K. Shukla,S. ShyamSundar,K. Siellez,M. Sieniawska,D. Sigg,Leo Singer,D. Singh,N. Singh,A. Singhal,Alicia M. Sintes,S. Sitmukhambetov,V. Skliris,B. J. J. Slagmolen,T. J. Slaven-Blair,J. R. Smith,Rory Smith,Surendra Nadh Somala,E. J. Son,S. Soni,B. Sorazu,Fiodor Sorrentino,T. Souradeep,E. Sowell,A. P. Spencer,Mario Spera,A. K. Srivastava,V. Srivastava,Kai Staats,C. Stachie,M. Standke,M. Standke,Daniele A. Steer,M. Steinke,M. Steinke,Jessica Steinlechner,Jessica Steinlechner,Sebastian Steinlechner,D. Steinmeyer,D. 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Vardaro,Vijay Varma,S. Vass,M. Vasúth,Alberto Vecchio,G. Vedovato,John Veitch,P. J. Veitch,K. Venkateswara,G. Venugopalan,D. Verkindt,F. Vetrano,A. Viceré,Aaron Viets,Serena Vinciguerra,D. J. Vine,J-Y. Vinet,Salvatore Vitale,T. Vo,H. Vocca,C. Vorvick,S. P. Vyatchanin,A. R. Wade,L. E. Wade,M. Wade,R. C. Walet,Michelle E. Walker,L. Wallace,S. Walsh,Hua Wang,Jianfang Wang,Shao-Jiang Wang,Wenxiao Wang,Yu Wang,R. L. Ward,Z. A. Warden,J. Warner,M. Was,Jennifer Watchi,B. Weaver,L.-W. Wei,L.-W. Wei,M. Weinert,M. Weinert,A. J. Weinstein,Rainer Weiss,Felix Wellmann,Felix Wellmann,Linqing Wen,E. K. Wessel,P. Weßels,P. Weßels,J. W. Westhouse,K. Wette,James Whelan,Bernard F. Whiting,C. Whittle,D. M. Wilken,D. M. Wilken,David A. Williams,A. R. Williamson,J. L. Willis,Benno Willke,Benno Willke,Walter Winkler,Walter Winkler,Christopher Wipf,H. Wittel,H. Wittel,Graham Woan,J. Woehler,J. Woehler,J. K. Wofford,J. L. Wright,D. S. Wu,D. S. Wu,Daniel Wysocki,S. Xiao,R. Xu,H. Yamamoto,C. C. Yancey,Lili Yang,Yang Yang,Z. Yang,M. J. Yap,Maher Yazback,D. W. Yeeles,Hang Yu,Haocun Yu,S. H. R. Yuen,A. K. Zadrożny,A. K. Zadrożny,M. Zanolin,T. Zelenova,J.-P. Zendri,Michael Zevin,J. Zhang,Lei Zhang,T. Zhang,Chunnong Zhao,Guoying Zhao,Mingliang Zhou,Zifan Zhou,Xing-Jiang Zhu,Aaron Zimmerman,Michael E Zucker,Michael E Zucker,J. Zweizig +1257 more
TL;DR: In this paper, the authors present the results of a search for long-duration gravitational-wave transients in the data from the Advanced LIGO second observation run; they search for 2-500 s duration in the 24-2048 Hz frequency band with minimal assumptions about signal properties such as waveform morphologies, polarization, sky location or time of occurrence.
Journal ArticleDOI
Theories of central engine for long gamma-ray bursts
TL;DR: In this paper, the central engine of long GRBs associated with hypernovae has been studied and several promising mechanisms such as black hole and magnetar formation have been discussed, as well as some more exotic models.
Journal ArticleDOI
Dimension dependence of numerical simulations on gravitational waves from protoneutron stars
Hajime Sotani,Tomoya Takiwaki +1 more
TL;DR: In this article, the eigenfrequencies of gravitational wave from the PNSs provided via the core-collapse supernovae, focusing on how the frequencies depend on the dimension of numerical simulations especially for the early phase after core bounce.
References
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The evolution and explosion of massive stars
TL;DR: In this article, the authors examined the current understanding of the lives and deaths of massive stars, with special attention to the relevant nuclear and stellar physics, and focused on their post-helium-burning evolution.
Journal ArticleDOI
The Progenitor stars of gamma-ray bursts
TL;DR: In this paper, the authors explore the evolution of very rapidly rotating massive stars, including stripped-down helium cores that might result from mergers or mass transfer in a binary, and single stars that rotate unusually rapidly on the main sequence.
Journal ArticleDOI
LIGO: The Laser Interferometer Gravitational-Wave Observatory
TL;DR: Laser Interferometric Gravitational-Wave Observatory (LIGO) as discussed by the authors is a project to detect and study gravitational waves of astrophysical origin, which holds the promise of testing general relativity in the strong-field regime, providing a new probe of exotic objects such as black hole and neutron stars, and uncovering unanticipated new astrophysics.
Journal ArticleDOI
Revival of a stalled supernova shock by neutrino heating
Hans A. Bethe,James R. Wilson +1 more
Journal ArticleDOI
LIGO: The laser interferometer gravitational-wave observatory
TL;DR: LIGO as discussed by the authors is a trio of extremely sensitive Michelson interferometers built to detect gravitational waves from space, and the results of their recent observations are described in detail.