The Yields of r-Process Elements and Chemical Evolution of the Galaxy

Chen, Zhe; Zhang, Jiang; Chen, Yanping; Cui, Wenyuan; Zhang, Bo

doi:10.1007/s10509-006-9229-2

Cited by 3 publications

(4 citation statements)

References 39 publications

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“…The conclusion drawn in S97, that is supported here, was that the mass of the star resulting in the Type II Supernova that produced the r-process element was insufficient to simultaneously produce the α-elements. The Ba and Eu abundances derived here fall within the range of values of collated data and model yields in Chen et al (2006). Based on this the two modes of M15 are both indicative of pollution by Type II supernova.…”

Section: Heavy and Light Element Contributions Within M15supporting

confidence: 77%

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Ba and Eu abundances in M 15 giant stars

Worley

Hill

Sobeck

et al. 2013

A&A

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Aims. We investigate the Ba and Eu abundances for a sample of 63 giant stars in the globular cluster M 15. This is the largest sample of M 15 giant stars for which Ba abundances have been determined and, due to the target selection of the original research programme, the Ba abundances are complete along the red giant branch. Methods. Stellar parameters were taken from the previous key study and a microturbulence-surface gravity relation was determined for precise measurement of the Ba line at 6496.898 Å, which has a high sensitivity to microturbulence. Element abundances for Ba, La, Eu, Ca, Ni and Fe were calculated using spectrum synthesis and equivalent widths techniques.

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Section: Heavy and Light Element Contributions Within M15supporting

confidence: 77%

“…Based on this the two modes of M15 are both indicative of pollution by Type II supernova. As concluded in Chen et al (2006) and references therein, Supernova Type II associated with stars of progenitor mass between 20 M ⊙ and 40 M ⊙ are the main source of r-process elements in the early galaxy.…”

Section: Heavy and Light Element Contributions Within M15mentioning

confidence: 79%

Ba and Eu abundances in M 15 giant stars

Worley

Hill

Sobeck

et al. 2013

A&A

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“…The results indicate that except for the earliest phase ([Fe/H] < −2.5) double compact star mergers contribute 12 The observations are taken from Woolf et al (1995), Burris et al (2000) and Chen et al (2006). significantly to the chemical enrichment of r-process elements of the Galaxy. This enrichment is mainly due to the BH+NS binary mergers, while the double NS binary mergers (and the NS+BH mergers) only contribute marginally.…”

Section: Resultsmentioning

confidence: 99%

Massive double compact object mergers: gravitational wave sources and r-process element production sites

Mennekens

Vanbeveren

2014

A&A

173

197

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With our galactic evolutionary code that contains a detailed intermediate-mass and massive binary population model, we study the temporal evolution of the galactic population of double neutron star binaries, mixed systems with a neutron star and black hole component, and double black hole binaries. We computed the merger rates of these relativistic binaries and translate them into LIGO II detection rates. We demonstrate that accounting for the uncertainties in the relation "initial mass-final mass" predicted by massive close binary evolution and due to the possible effect of large stellar wind mass loss during the luminous blue variable phase of a star with initial mass higher than 30−40 M and during the red supergiant phase of a star with initial mass lower than 30−40 M when such a star is a binary component, the double black hole merger rate may be very low, contrary to predictions made by other groups. Hydrodynamic computations of the r-process chemical yields ejected during the relativistic binary merger process have recently become available. With our galactic code that includes binaries, it is then straightforward to calculate the temporal galactic evolution of the r-process elements ejected by these mergers. We conclude that except for the earliest evolutionary phase of the Galaxy (∼the first 100 Myr), double compact star mergers may be the major production sites of r-process elements, and it is probable that the mixed systems dominate this production over double neutron star binary mergers.

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“…These are produced only by the rapid neutron capture process (r-process) acting on the iron-peak isotopes. This is thought to occur only during explosive nucleosynthesis in stars with 10−20M (Chen et al 2006). In contrast, Si is produced during α-chain process by the whole range of massive stars.…”

Section: Initial Bulk-chemistry and Initial Radiogenic-power Variationsmentioning

confidence: 99%

Geodynamics and Rate of Volcanism on Massive Earth-Like Planets

Kite

Manga

Gaidos

2009

ApJ

165

175

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We provide estimates of volcanism versus time for planets with Earth-like composition and masses 0.25 -25 M ⊕ , as a step toward predicting atmospheric mass on extrasolar rocky planets. Volcanism requires melting of the silicate mantle. We use a thermal evolution model, calibrated against Earth, in combination with standard melting models, to explore the dependence of convection-driven decompression mantle melting on planet mass. We show that (1) volcanism is likely to proceed on massive planets with plate tectonics over the main-sequence lifetime of the parent star; (2) crustal thickness (and melting rate normalized to planet mass) is weakly dependent on planet mass; (3) stagnant lid planets live fast (they have higher rates of melting than their plate tectonic counterparts early in their thermal evolution), but die young (melting shuts down after a few Gyr); (4) plate tectonics may not operate on high mass planets because of the production of buoyant crust which is difficult to subduct; and (5) melting is necessary but insufficient for efficient volcanic degassing -volatiles partition into the earliest, deepest melts, which may be denser than the residue and sink to the base of the mantle on young, massive planets. Magma must also crystallize at or near the surface, and the pressure of overlying volatiles must be fairly low, if volatiles are to reach the surface. If volcanism is detected in the τ Ceti system, and tidal forcing can be shown to be weak, this would be evidence for plate tectonics.

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The Yields of r-Process Elements and Chemical Evolution of the Galaxy

Cited by 3 publications

References 39 publications

Ba and Eu abundances in M 15 giant stars

Ba and Eu abundances in M 15 giant stars

Massive double compact object mergers: gravitational wave sources and r-process element production sites

Geodynamics and Rate of Volcanism on Massive Earth-Like Planets

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