Nonlinear growth of Rayleigh-Taylor instabilities and mixing in SN 1987A

Hachisu, Izumi; Matsuda, Takuya; Nomoto, Ken’ichi; Shigeyama, Toshikazu

doi:10.1086/185779

Cited by 139 publications

(131 citation statements)

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“…The processed material is assumed to mix uniformly in the region from M r = 1.8 M ⊙ to 6.0 M ⊙ (where M r denotes the lagrangian mass coordinate measured from the centre of the pre-supernova model). Such a large-scale mixing was found to take place in SN1987A and various explosion models 15,16 . Almost all materials below M r = 6.0M ⊙ falls back to the central remnant and only a small fraction (factor f = 2 ×10 −5 ) is ejected from this region.…”

mentioning

confidence: 88%

First-generation black-hole-forming supernovae and the metal abundance pattern of a very iron-poor star

Umeda

Nomoto

2003

Nature

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407

391

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It has been proposed 1 theoretically that the first generation of stars in the Universe (population III) would be as massive as 100 solar masses (100M ⊙ ), because of inefficient cooling 2−4 of the precursor gas clouds. Recently, the most iron-deficient (but still carbon-rich) low-mass star -HE0107-5240 -was discovered 5 . If this is a population III that gained its metals (elements heavier than helium) after its formation, it would challenge the theoretical picture of the formation of the first stars. Here we report that the patterns of elemental abundance in HE0107-5240 (and other extremely metal-poor stars) are in good accord with the nucleosynthesis that occurs in stars with masses of 20 − 130M ⊙ when they become supernovae if, during the explosions, the ejecta undergo substantial mixing and fall-back to form massive black holes. Such supernovae have been observed 7 . The abundance patterns are not, however, consistent with enrichment by supernovae from stars in the range 130 − 300M ⊙ . We accordingly infer that the first-generation supernovae came mostly from explosions of ∼ 20 − 130M ⊙ stars; some of these produced iron-poor but carbon-and oxygen-rich ejecta. Low-mass second-generation stars, like HE0107-5240, could form because the carbon and oxygen provided pathways for gas to cool.The abundance pattern of HE0107-5240 is characterized by very large C/Fe and N/Fe ratios, while the abundances of elements heavier than Mg are as low as that of Fe (Fig. 1). How could this peculiar abundance pattern have be formed? We note that this is not the only extremely metal-poor (EMP) star to have large C/Fe and N/Fe ratios -several other such stars have been discovered 8−10 .Therefore a reasonable explanation of the abundance pattern should also apply to other EMP stars.Before describing our model, we examine two alternative explanations of the abundance pattern of C-rich EMP stars 5 . These explanations assume that small-mass stars formed from EMP gases, and that carbon was enhanced after the formation. The first is mass transfer from a companion star.

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confidence: 88%

First-generation black-hole-forming supernovae and the metal abundance pattern of a very iron-poor star

Umeda

Nomoto

2003

Nature

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407

391

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“…Model IIP20: The R-T instability is weak at the He/C+O interface as found in the model for SN 1987A (Hachisu et al 1990(Hachisu et al , 1992, but it grows at the H/He interface. The development of R-T instabilities in this II-P model is somewhat different from SN 1987A.…”

Section: Type Ii-p Supernovaementioning

confidence: 64%

“…This has stimulated 2D and 3D hydrodynamical calculations of the Rayleigh-Taylor (R-T) instabilities during supernova explosions for SN1987A (Arnett et al 1989;Hachisu et al 1990Hachisu et al , 1992Fryxell et al 1991;Miiller et al 1991;Den et al 1990;Yamada et al 1990;Yamada & Sato 1991;Herant & Benz 1991, type Ib/Ic supernovae (Hachisu et al , 1994a, type II-P supernovae (Herant &: Woosley 1994;Hachisu et al 1994b), and the type Il-b supernova 1993J (Iwamoto et al 1994). In particular, Hachisu et al ( , 1994a found that development of the R-T instabilities depend sensitively on the presupernova structure, so that the comparison between hydrodynamical simulations and observations can provide a new clue to the understanding of supernova progenitors, their structure, and the explosion mechanism.…”

Section: Introductionmentioning

confidence: 99%

Instabilities and Mixing in Type II-P and II-b Supernovae

Shigeyama

Iwamoto

Hachisu

et al. 1996

International Astronomical Union Colloquium

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“…Observations of SN1987A highlighted two distinct defects with these models. [55] One means of evaluating SN models is through the light curve, the total luminosity of the SN versus time. The SN luminosity decreases sharply imme&ately after the explosion as ejected gas hydrodynamically cools due to expansion.…”

Section: Sn1987a MIX Exnerimentsmentioning

confidence: 99%

Laboratory measurements of materials in extreme conditions: the use of high energy radiation sources for high pressure studies

Cauble¹,

Remington²,

Campbell³

1999

International Journal of Impact Engineering

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High energy lasers can be used to study material conditions that are appropriate fort inertial confinement fusion: that is, materials at high densities, temperatures, and pressures. Pulsed power devices can offer similar opportunities. The National Ignition Facility (NIP) will be a high energy multi-beam laser designed to achieve the thermonuclear ignition of a mm-scale DT-fried target in the laboratory. At the same time, NE will provide the physics community with a unique tool for the study of high energy density matter at states unreachable by any other laboratory technique. Here we describe how these lasers and pulsed power tools can contribute to investigations of high energy density matter in the areas of material properties and equations of state, extend present laboratory shock techniques such as high-speed jets to new regimes, and allow study of extreme conditions found in astrophysical phenomenaThe purpose of this article is to introduce and describe the kinds of high energy density experiments that are now being done with high energy radiation sources --lasers and pulsed power devices --on present-day facilities and to indicate where these investigations might proceed with larger facilities either on the drawing board or under construction. Both pulsed power and laser facilities have been funded predominantly for research i,n inertial confinement fusion (KF) or, in the case ofpulsed power% as high flux, short wavelength x-ray sources. The idea that they could be used to investigate specific areas of high energy density physics took some time to germinate, The growth of physics-specific experiments on lasers and pulsed power has been driven largely by the need for high energy density information in the absence of nuclear testing.Although the use of high energy lasers for studies of, e.g., material properties at extremely high pressure or high-Mach-number hydrodynamic flow, is recent --less than 10 years, the use of pulsed power machines for such experiments is even newer. Since there is a base of laser experiments on facilities like Nova at Lawrence Livermore National Laboratory (LLNL), the bulk of this article will discuss those experiments. Pulsed power facilities like Z at Sandia National Laboratories (SNL) can and will perform measurements similar to those described below. Extensions of Nova experiments to next generation lasers, like the National Ignition Facility (to be bui1.t at LLNL) can be made. The next generation pulsed power machine, designated X-l, may be built at SNL in the next century.Lasers and pulsed power devices can produce high energy radiation sources but can be seen as somewhat complementary. The most energetic laser for the past 15 years has been Nova[ I], although the B&EGA laser[Z!] at the University of Rochester is now equivalent. Nova is a tenbeam laser that can produce about 1.00 kJ of l-pm-wavelength laser light. This long wavelength,

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Nonlinear growth of Rayleigh-Taylor instabilities and mixing in SN 1987A

Cited by 139 publications

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First-generation black-hole-forming supernovae and the metal abundance pattern of a very iron-poor star

First-generation black-hole-forming supernovae and the metal abundance pattern of a very iron-poor star

Instabilities and Mixing in Type II-P and II-b Supernovae

Laboratory measurements of materials in extreme conditions: the use of high energy radiation sources for high pressure studies

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