Atomic data for opacity calculations. XXIII. The aluminium isoelectronic sequence

Mendoza, C.; Eissner, W.; Dourneuf, M. Le; Zeippen, C. J.

doi:10.1088/0953-4075/28/16/006

Cited by 76 publications

(69 citation statements)

References 64 publications

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“…In addition to the primary sources listed above, the atomic data for the present calculations were taken from Shine & Linsky (1974), Mendoza (1983), Nussbaumer & Storey (1983), Nussbaumer & Storey (1984), Luo & Pradhan (1989), Cunto et al (1993), Nahar & Pradhan (1993), Butler et al (1993), Zhang & Pradhan (1994), Nahar & Pradhan (1994), Mendoza et al (1995), Zhang & Pradhan (1995a), Zhang & Pradhan (1995b), Zhang (1996), Fernley et al (1999, Sunderland et al (2002), Tachiev &Froese Fischer (2002), andBautista (2004).…”

Section: Appendix A: Details On the Radiative Transfer Calculations Amentioning

confidence: 99%

Inferring supernova IIb/Ib/Ic ejecta properties from light curves and spectra: correlations from radiative-transfer models

Dessart¹,

Hillier²,

Woosley³

et al. 2016

Mon. Not. R. Astron. Soc.

139

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We present 1-D non-Local-Thermodynamic-Equilibrium time-dependent radiative-transfer simulations for a large grid of supernovae (SNe) IIb/Ib/Ic that result from the terminal explosion of the mass donor in a close-binary system. Our sample covers ejecta masses M e of 1.7-5.2 M d , kinetic energies E kin of 0.6-5.0ˆ10 51 erg, and 56 Ni masses of 0.05-0.30 M d . We find a strong correlation between the 56 Ni mass and the photometric properties at maximum, and between the rise time to bolometric maximum and the post-maximum decline rate. We confirm the small scatter in (V´R) at 10 d past R-band maximum. The quantity V m " a 2E kin {M e is comparable to the Doppler velocity measured from He I 5875Å at maximum in SNe IIb/Ib, although some scatter arises from the uncertain level of chemical mixing.The O I 7772Å line may be used for SNe Ic, but the correspondence deteriorates with higher ejecta mass/energy. We identify a temporal reversal of the Doppler velocity at maximum absorption in the " 1.05 µm feature in all models. The reversal is due to He I alone and could serve as a test for the presence of helium in SNe Ic. Because of variations in composition and ionisation, the ejecta opacity shows substantial variations with both velocity and time. This is in part the origin of the offset between our model light curves and the predictions from the Arnett model.

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Section: Appendix A: Details On the Radiative Transfer Calculations Amentioning

confidence: 99%

Inferring supernova IIb/Ib/Ic ejecta properties from light curves and spectra: correlations from radiative-transfer models

Dessart¹,

Hillier²,

Woosley³

et al. 2016

Mon. Not. R. Astron. Soc.

139

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“…They have accuracy grades of B+ and A+. For the higher nl levels, we list theoretical data from Mendoza et al (1995), which were determined by non-relativistic R-matrix calculations. Furthermore, their data for finestructure levels were derived from the multiplet values assuming a pure LS-coupling.…”

Section: Aluminum Speciesmentioning

confidence: 99%

Atomic Data Revisions for Transitions Relevant to Observations of Interstellar, Circumgalactic, and Intergalactic Matter

Cashman

Kulkarni

Kisielius

et al. 2017

ApJS

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Measurements of element abundances in galaxies from astrophysical spectroscopy depend sensitively on the atomic data used. With the goal of making the latest atomic data accessible to the community, we present a compilation of selected atomic data for resonant absorption lines at wavelengths longward of 911.753Å (the H I Lyman limit), for key heavy elements (heavier than atomic number 5) of astrophysical interest. In particular, we focus on the transitions of those ions that have been observed in the Milky Way interstellar medium (ISM), the circumgalactic medium (CGM) of the Milky Way and/or other galaxies, and the intergalactic medium (IGM). We provide wavelengths, oscillator strengths, associated accuracy grades, and references to the oscillator strength determinations. We also attempt to compare and assess the recent oscillator strength determinations. For about 22% of the lines that have updated oscillator strength values, the differences between the former values and the updated ones are 0.1 dex. Our compilation will be a useful resource for absorption line studies of the ISM, as well as studies of the CGM and IGM traced by sight lines to quasars and gamma-ray bursts. Studies (including those enabled by future generations of extremely large telescopes) of absorption by galaxies against the light of background galaxies will also benefit from our compilation.

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“…Tfie situation for Al 1 is similar Tfie NIST-ASD recommends primarily OP results [39]. Many of tfie important multiplets involve a single valence electron cfianging its orbit outside of a closed 3s^ sub-sfieU.…”

Section: Some Remaining Analytical Issuesmentioning

confidence: 82%

An Observational Perspective on Some Aspects of Early Stellar Nucleosynthesis

Sneden¹,

Lawler

2008

AIP Conference Proceedings

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Abstract. Some basic abundance results for low metallicity stars that were formed in the early days of the Milky Way Galaxy are summarized. Discussion is centered on two nucleosynthetic groups: the light a elements (Mg, Si, and Ca), and the neutroncapture elements (those heavier than the Fe group, atomic numbers greater than 30). Emphasis is placed on the present state of stellar spectroscopic and atomic transition data.Keywords: stellar abundances, low metallicity stars, nucleosynthesis PACS: 26.30.+k,95.30,95.75,95.85.Kr,95.85.Ls,97

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Atomic data for opacity calculations. XXIII. The aluminium isoelectronic sequence

Cited by 76 publications

References 64 publications

Inferring supernova IIb/Ib/Ic ejecta properties from light curves and spectra: correlations from radiative-transfer models

Inferring supernova IIb/Ib/Ic ejecta properties from light curves and spectra: correlations from radiative-transfer models

Atomic Data Revisions for Transitions Relevant to Observations of Interstellar, Circumgalactic, and Intergalactic Matter

An Observational Perspective on Some Aspects of Early Stellar Nucleosynthesis

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