4.4 Abundances of the elements in the Solar System

Lodders, K.; Palme, H.; Gail, H. P.

doi:10.1007/978-3-540-88055-4_34

Cited by 763 publications

(1,074 citation statements)

References 107 publications

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“…The total luminosities (summed over the three temperature components) in other energy bands (0.5-4 keV, 0.1-2.4 keV, and 0.4-4 keV) for Einstein, ROSAT, ASCA given in the papers by Cassinelli & Swank (1983), Haberl &White (1993), andCorcoran et al (1994), respectively, do agree with our values when taking differences in interstellar absorption or distance into account. The abundances are relative to solar photospheric values (Lodders et al 2009). The absolute values of the abundances are strongly influenced by the obtained values of the emission measures.…”

Section: A 3-t Modelmentioning

confidence: 99%

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The X-ray spectrum ofδOrionis observed by LETGS aboardChandra

Raassen

Pollock

2013

A&A

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Aims. We analyze the high-resolution X-ray spectrum of the supergiant O-star δ Orionis (O9.5II) with line ratios of He-like ions and a thermal plasma model, and we examine its variability. Methods. The O-supergiant δ Ori was observed in the wavelength range 5-175 Å by the X-ray detector HRC-S in combination with the grating LETG aboard Chandra. We studied the He-like ions in combination with the UV-radiation field to determine local plasma temperatures and to establish the distance of the X-ray emitting ions to the stellar surface. We measured individual lines by means of Gaussian profiles, folded through the response matrix, to obtain wavelengths, line fluxes, half widths at half maximum (HWHM) and line shifts to characterize the plasma. We consider multitemperature models in collisional ionization equilibrium (CIE) to determine temperatures, emission measures, and abundances.Results. Analysis of the He-like triplets extended to N vi and C v implies ionization stratification with the hottest plasma to be found within a few stellar radii 3 R * (Mg xi) and the coolest farther out, far beyond the acceleration zone, up to 49 R * (N vi) and 75 R * (C v).The observed temperatures cover a range from about 0.1 to 0.7 keV, i.e., 1-8 MK. The X-ray luminosity (L x ) is ∼1.5 × 10 32 erg/s in the range from 0.07 to 3 keV covered by LETGS. Velocity widths of about 1040 km s −1 have been determined.

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Section: A 3-t Modelmentioning

confidence: 99%

“…The obtained abundances are relative to solar photospheric values (Lodders et al 2009). They were fit by fixing the iron abundance at its solar photospheric value and leaving the carbon, nitrogen, oxygen, neon, magnesium, and silicon abundances free to vary.…”

mentioning

confidence: 99%

The X-ray spectrum ofδOrionis observed by LETGS aboardChandra

Raassen

Pollock

2013

A&A

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“…1). The allowed region inferred from the 244 Pu abundance in the deep-sea floor [9] and the ESS [10,13] is shown as a blue region. The blue solid (dotted) line corresponds to the current ISM 244 Pu density being the median (2σ) value.…”

Section: Total Heavy R-process Production In the Milky Waymentioning

confidence: 99%

“…The relative abundance ratio of ( 244 Pu/ 238 U) ESS ≈ 0.008 is estimated from fissiogenic xenon in ESS material [10]. Y U, ESS = 7.3×10 −13 is the number abundance of 238 U relative to hydrogen inferred from meteorites ( [13] ; corrected from the present for 238 U decay) and n ISM is the mean number density of the ISM, which is typically ≈ 1 cm −3 .…”

Section: Measured Short Lived 244 Pu Abundancesmentioning

confidence: 99%

Short-Lived ²⁴⁴Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis

Hotokezaka¹,

Piran²,

Paul³

2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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Measurements of the radioactive 244 Pu abundances can break the degeneracy between high-rate/lowyield and low-rate/high-yield scenarios for the production of heavy r-process elements. The first corresponds to production by core collapse supernovae (cc-SNe) while the latter corresponds to production by e.g. neutron star binary mergers. The estimated 244 Pu abundance in the current interstellar medium inferred from deep-sea measurements is significantly lower than that corresponding Early Solar System abundances. We estimate the expected median value of the 244 Pu abundances and fluctuations around this value in both models [1]. We show that while the current and Early Solar System abundances are explained within the low-rate/high-yield scenario, they are incompatible with the high-rate/low-yield (cc-SNe) model. The inferred event rate remarkably agrees with neutron star binary merger rates estimated from Galactic neutron star binaries and from short gamma-ray bursts. The ejected mass of r-process elements per event agrees with both theoretical and observational macronova estimates.

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“…with T 1/2 < 10 9 yr are considered to be completely decayed, which is the reason for the large [ 40 K/Fe] value (T 1/2 ( 40 K) = 1.28 × 10 9 yr). The solar abundances are from Lodders et al (2009) [5].…”

Section: Ejection Criteriamentioning

confidence: 99%

Nucleosynthesis in 2D Core-Collapse Supernova Long-Term Simulations of 11.2 and 17.0 \(\text{M}_{ \odot }\) Progenitors

Eichler¹,

Nakamura²,

Takiwaki³

et al. 2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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We perform detailed nucleosynthesis calculations for two long-term, 2D simulations of core-collapse supernovae. We find that elements are produced up to Ru (Z = 44) and observe abundance patterns that are characteristic of a νp-process. One important characteristic of the long-term simulation is that there is still accretion of matter onto the proto-neutron star and unbinding of matter in some other regions at the time when the simulations stop (around 7s). Dividing the tracer particles into different bins according to their peak temperatures enables us to study and compare the nuclear compositions of these bins for the different simulations.

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4.4 Abundances of the elements in the Solar System

Cited by 763 publications

References 107 publications

The X-ray spectrum ofδOrionis observed by LETGS aboardChandra

The X-ray spectrum ofδOrionis observed by LETGS aboardChandra

Short-Lived ²⁴⁴Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis

Nucleosynthesis in 2D Core-Collapse Supernova Long-Term Simulations of 11.2 and 17.0 \(\text{M}_{ \odot }\) Progenitors

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4.4 Abundances of the elements in the Solar System

Cited by 763 publications

References 107 publications

The X-ray spectrum ofδOrionis observed by LETGS aboardChandra

The X-ray spectrum ofδOrionis observed by LETGS aboardChandra

Short-Lived 244Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis

Nucleosynthesis in 2D Core-Collapse Supernova Long-Term Simulations of 11.2 and 17.0 \(\text{M}_{ \odot }\) Progenitors

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Short-Lived ²⁴⁴Pu Points to Neutron Star Binary Mergers as Sites for r-Process Nucleosynthesis