Stellar Origin of <sup>15</sup>N-rich Presolar SiC Grains of Type AB: Supernovae with Explosive Hydrogen Burning

Liu, Nan; Nittler, L. R.; Pignatari, M.; Alexander, Conel M. O'd.; Wang, Jingyuan

doi:10.3847/2041-8213/aa74e5

Cited by 59 publications

(78 citation statements)

References 37 publications

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“…However, as will be shown later, these three AB2 grains had near-normal Mo isotopic compositions as the other nine AB2 grains, but different from the anomalous Mo isotopic compositions observed in most of the MS grains, which thus supports the relaxation of the AB grain definition as also suggested by Liu et al (2017).…”

Section: Methodssupporting

confidence: 66%

“…SiC grains on the three mounts were identified by automated BSE (backscattered electron)-EDX (energy-dispersive X-ray) analysis (Liu et al 2016a). Isotopic analysis of C, N, and Si in the AB2 and MS grains was performed with the NanoSIMS 50L ion microprobe at the Carnegie Institution using standard procedures (Liu et al 2016b(Liu et al , 2017. All data were collected in the imaging mode, with ~150 nm spatial resolution, which allowed selection of smaller regions of interest during data reduction to minimize potential contamination.…”

Section: Methodsmentioning

confidence: 99%

“…In contrast, the AB2 grains in this study show neutroncapture signatures that are even weaker than the s-process signatures and are thus inconsistent with being from born-again AGB stars (Liu et al 2014b). It should be pointed out that none of the AB1 grains have been clearly demonstrated to have come from born-again AGB stars (Liu et al 2016b(Liu et al , 2017. On the other hand, the graphite grains that have been assigned to a born-again AGB stellar origin (Jadhav et al 2013) could be alternatively explained by nucleosynthesis in supernovae with H ingestion (Liu et al 2017).…”

Section: Potential Stellar Origin(s) Of Ab2 Grainsmentioning

confidence: 99%

“…The AB grains were initially divided into two groups, A and B (Hoppe et al 1994; 12 C/ 13 C A <3.5≤ 12 C/ 13 C B ≤10), which were subsequently combined as a single group with 12 C/ 13 C≤10 due to the lack of any other obvious differences (Amari et al 2001). A recent study of AB grains (Liu et al 2017) has shown distinctive differences in the isotopic compositions of C, N, Al, and Si between 15 N-rich ( 14 N/ 15 N ≤ 440, the solar ratio, AB1 group) and 14 N-rich ( 14 N/ 15 N > 440, AB2 group) AB grains, thus suggesting different stellar sources of these two subgroups. Liu et al (2017) found that AB1 grains (2−3% of all SiC) show an anticorrelation between their 14 N/ 15 N and their inferred 26 Al/ 27 Al ratios, which points to an origin in supernovae, in which H was ingested into the He/C zones prior to the explosions.…”

Section: Introductionmentioning

confidence: 99%

“…A recent study of AB grains (Liu et al 2017) has shown distinctive differences in the isotopic compositions of C, N, Al, and Si between 15 N-rich ( 14 N/ 15 N ≤ 440, the solar ratio, AB1 group) and 14 N-rich ( 14 N/ 15 N > 440, AB2 group) AB grains, thus suggesting different stellar sources of these two subgroups. Liu et al (2017) found that AB1 grains (2−3% of all SiC) show an anticorrelation between their 14 N/ 15 N and their inferred 26 Al/ 27 Al ratios, which points to an origin in supernovae, in which H was ingested into the He/C zones prior to the explosions. In comparison, AB2 grains (2−3% of all SiC) do not show any correlation between their N and Al isotope ratios, and their stellar origins remain unclear.…”

Section: Introductionmentioning

confidence: 99%

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J-type Carbon Stars: A Dominant Source of ¹⁴N-rich Presolar SiC Grains of Type AB

Liu

Stephan

Boehnke

et al. 2017

ApJL

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We report Mo isotopic data of 27 new presolar SiC grains, including 12 14 N-rich AB ( 14 N/ 15 N > 440, AB2) and 15 mainstream (MS) grains, and their correlated Sr and Ba isotope ratios when available. Direct comparison of the data for the MS grains, which came from lowmass asymptotic giant branch (AGB) stars with large s-process isotope enhancements, with the AB2 grain data demonstrates that AB2 grains show near-solar isotopic compositions and lack sprocess enhancements. The near-normal Sr, Mo, and Ba isotopic compositions of AB2 grains clearly exclude born-again AGB stars, where the intermediate neutron-capture process (iprocess) takes place, as their stellar source. On the other hand, low-mass CO novae, and early Rand J-type carbon stars show 13 C and 14 N excesses but no s-process enhancements and are thus potential stellar sources of AB2 grains. Since both early R-type carbon stars and CO novae are rare objects, the abundant J-type carbon stars (10−15% of all carbon stars) are thus likely to be a dominant source of AB2 grains.

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Section: Methodssupporting

confidence: 66%

Section: Methodsmentioning

confidence: 99%

Section: Potential Stellar Origin(s) Of Ab2 Grainsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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J-type Carbon Stars: A Dominant Source of ¹⁴N-rich Presolar SiC Grains of Type AB

Liu

Stephan

Boehnke

et al. 2017

ApJL

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Presolar SiC Grains of Type AB with Isotopically Light Nitrogen: Contributions from Supernovae?

Hoppe

Pignatari

Amari³

2019

Springer Proceedings in Physics

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Massive Stars and Their Supernovae

Thielemann¹,

Diehl²,

Heger³

et al. 2018

Astrophysics With Radioactive Isotopes

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Our understanding of stellar evolution and the final explosive endpoints such as supernovae or hypernovae or gamma-ray bursts relies on the combination of a) (magneto-)hydrodynamics b) engergy generation due to nuclear reactions accomanying composition changes c) radiation transport d) thermodynamic properties (such as the equation of state of stellar matter).Hydrodynamics is essentially embedded within the numerical schemes which implement the physics of processes (b) to (d). In early phases of stellar evolution, hydrodynamical processes can be approximated by a hydrostatic treatment. Nuclear energy production (b) includes all nuclear reactions triggered during stellar evolution and explosive end stages, also among unstable isotopes produced on the way. Radiation transport (c) covers atomic physics (e.g. opacities) for photon transport, but also nuclear physics and neutrino nucleon/nucleus interactions in late phases and core collapse. The thermodynamical treatment (d) addresses the mixture of ideal gases of photons, electrons/positrons and nuclei/ions. These are fermions and bosons, in dilute media or at high temperatures their energies can often be approximated by Maxwell-Boltzmann distributions. At very high densities, the nuclear equation of state is required to relate pressure and density. It exhibits a complex behavior, with transitions from individual nuclei to clusters of nucleons with a background neutron bath, homogeneous phases of nucleons, the emergence of hyperons and pions up to a possible hadron-quark phase transition.The detailed treatment of all these ingredients and their combined application is discussed in more depth in textbooks (Kippenhahn and Weigert, 1994; Maeder, /or the preceding Chapter (3), where the evolution of low and intermediate mass stars is addressed. That chapter also includes the stellar structure equations in spherical symmetry and a discussion of opacities for photon transport. Ch. 8 and 9 (tools for modeling objects and their processes) go into more detail with regard to modeling hydrodynamics, (convective) instabilities and energy transport as well as the energy generation due to nuclear reactions and the determination of the latter. Here we want to focus on the astrophysical aspects, i.e. a description of the evolution of massive stars and their endpoints with a special emphasis on the composition of their ejecta (in form of stellar winds during the evolution or of explosive ejecta). Low and intermediate mass stars end their evolution as AGB stars, finally blowing off a planetary nebula via wind losses and leaving a white dwarf with an unburned C and O composition. Massive stars evolve beyond this point and experience all stellar burning stages from H over He, C, Ne, O and Si-burning up to core collapse and explosive endstages. In this chapter we want to discuss the nucleosynthesis processes involved and the production of radioactive nuclei 5 in more detail. This includes all hydrostatic nuclear-burning stages experienced by massive stars, and explosive burning stages wh...

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Stellar Origin of ¹⁵N-rich Presolar SiC Grains of Type AB: Supernovae with Explosive Hydrogen Burning

Abstract: We report C, N, and Si isotopic data for 59 highly 13 C-enriched presolar submicron-to

Cited by 59 publications

References 37 publications

J-type Carbon Stars: A Dominant Source of ¹⁴N-rich Presolar SiC Grains of Type AB

J-type Carbon Stars: A Dominant Source of ¹⁴N-rich Presolar SiC Grains of Type AB

Presolar SiC Grains of Type AB with Isotopically Light Nitrogen: Contributions from Supernovae?

Massive Stars and Their Supernovae

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Stellar Origin of 15N-rich Presolar SiC Grains of Type AB: Supernovae with Explosive Hydrogen Burning

Abstract: We report C, N, and Si isotopic data for 59 highly 13 C-enriched presolar submicron-to

Cited by 59 publications

References 37 publications

J-type Carbon Stars: A Dominant Source of 14N-rich Presolar SiC Grains of Type AB

J-type Carbon Stars: A Dominant Source of 14N-rich Presolar SiC Grains of Type AB

Presolar SiC Grains of Type AB with Isotopically Light Nitrogen: Contributions from Supernovae?

Massive Stars and Their Supernovae

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Stellar Origin of ¹⁵N-rich Presolar SiC Grains of Type AB: Supernovae with Explosive Hydrogen Burning

J-type Carbon Stars: A Dominant Source of ¹⁴N-rich Presolar SiC Grains of Type AB

J-type Carbon Stars: A Dominant Source of ¹⁴N-rich Presolar SiC Grains of Type AB