Stellar Collapse and Gravitational Waves

Fryer, Chris L.; Holz, D. E.; Hughes, Scott A.; Warren, Michael S.

doi:10.1007/978-0-306-48599-2_13

Cited by 9 publications

(13 citation statements)

References 25 publications

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“…Furthermore, they found that the host galaxies of the GRBs are significantly fainter and more irregular than the hosts of the supernovae. Theoretical work (Fryer 2004(Fryer , 2006 shows that stars which started out on the main sequence with masses between 8 and 20 M leave neutron stars as remnants, while the cores of stars more massive than about 20 M collapse to black holes. Figure 1, after Fryer (2006) shows that this happens irrespective of initial metallicity, although the black holes produced at lower metallicity tend to be much more massive than those from higher Fryer (2006) metallicity stars.…”

Section: Host Galaxy Characteristics: Further Evidence For An Associamentioning

confidence: 99%

Long gamma-ray burst progenitors: boundary conditions and binary models

Heuvel

Yoon

2007

Astrophys Space Sci

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The observed association of Long Gamma-Ray Bursts (LGRBs) with peculiar Type Ic supernovae gives support to Woosley's collapsar/hypernova model, in which the GRB is produced by the collapse of the rapidly rotating core of a massive star to a black hole. The association of LGRBs with small star-forming galaxies suggests low-metallicity to be a condition for a massive star to evolve to the collapsar stage. Both completely-mixed single star models and binary star models are possible. In binary models the progenitor of the GRB is a massive helium star with a close companion. We find that tidal synchronization during core-helium burning is reached on a short timescale (less than a few millennia). However, the strong core-envelope coupling in the subsequent evolutionary stages is likely to rule out helium stars with main-sequence companions as progenitors of hypernovae/GRBs. On the other hand, helium stars in close binaries with a neutron-star or black-hole companion can, despite the strong core-envelope coupling in the post-helium burning phase, retain sufficient core angular momentum to produce a hypernova/GRB.

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Section: Host Galaxy Characteristics: Further Evidence For An Associamentioning

confidence: 99%

Long gamma-ray burst progenitors: boundary conditions and binary models

Heuvel

Yoon

2007

Astrophys Space Sci

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“…A precise definition of SNIb/Ic has since varied over the years (see Fryer 2004;Gray & Corbally 2009). Some interpretations assume hydrogen is absent for SNI "by definition of being typeI" (cf.…”

Section: Introductionmentioning

confidence: 99%

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

Parrent

Milisavljević

Söderberg

et al. 2016

ApJ

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Here we revisit line identifications of type I supernovae (SNe I) and highlight trace amounts of unburned hydrogen as an important free parameter for the composition of the progenitor. Most one-dimensional stripped-envelope models of supernovae indicate that observed features near 6000-6400 Å in typeI spectra are due to more than Si IIλ6355. However, while an interpretation of conspicuous Si IIλ6355 can approximate 6150 Å absorption features for all SNe Ia during the first month of free expansion, similar identifications applied to 6250 Å features of SNe Ib and Ic have not been as successful. When the corresponding synthetic spectra are compared with highquality timeseries observations, the computed spectra are frequently too blue in wavelength. Some improvement can be achieved with Fe II lines that contribute redward of 6150 Å; however, the computed spectra either remain too blue or the spectrum only reaches a fair agreement when the rise-time to peak brightness of the model conflicts with observations by a factor of two. This degree of disagreement brings into question the proposed explosion scenario. Similarly, a detection of strong Si IIλ6355 in the spectra of broadlined Ic and super-luminous events of type I/R is less convincing despite numerous model spectra used to show otherwise. Alternatively, we suggest 6000-6400 Å features are possibly influenced by either trace amounts of hydrogen or blueshifted absorption and emission in Hα, the latter being an effect which is frequently observed in the spectra of hydrogen-rich, SNe II.

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“…Strong GWs can be emitted during a gravitational collapse/explosion and, following the collapse, by the resulting compact remnant [309, 205, 206, 88, 269, 108, 150]. GW emission during the collapse itself may result if the collapse or explosion involves aspherical bulk mass motion or convection.…”

Section: Introductionmentioning

confidence: 99%

“…Core-collapse supernovae, in particular, have been investigated as sources of gravitational radiation for nearly four decades (see, e.g., [251, 311, 253, 64, 204, 89, 201, 350, 245, 106, 108, 67, 68, 165, 232]). However, during this time research has produced estimates of GW strength that vary over orders of magnitude.…”

Section: Introductionmentioning

confidence: 99%

Gravitational Waves from Gravitational Collapse

Fryer

New

2011

Living Rev. Relativ.

Self Cite

166

111

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Gravitational-wave emission from stellar collapse has been studied for nearly four decades. Current state-of-the-art numerical investigations of collapse include those that use progenitors with more realistic angular momentum profiles, properly treat microphysics issues, account for general relativity, and examine non-axisymmetric effects in three dimensions. Such simulations predict that gravitational waves from various phenomena associated with gravitational collapse could be detectable with ground-based and space-based interferometric observatories. This review covers the entire range of stellar collapse sources of gravitational waves: from the accretion-induced collapse of a white dwarf through the collapse down to neutron stars or black holes of massive stars to the collapse of supermassive stars.Electronic Supplementary MaterialSupplementary material is available for this article at 10.12942/lrr-2011-1.

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Stellar Collapse and Gravitational Waves

Cited by 9 publications

References 25 publications

Long gamma-ray burst progenitors: boundary conditions and binary models

Long gamma-ray burst progenitors: boundary conditions and binary models

LINE IDENTIFICATIONS OF TYPE I SUPERNOVAE: ON THE DETECTION OF Si II FOR THESE HYDROGEN-POOR EVENTS

Gravitational Waves from Gravitational Collapse

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