A parallel R-matrix program PRMAT for electron–atom and electron–ion scattering calculations

Sunderland, A.G.; Noble, C. J.; Burke, V.M.; Burke, P G

doi:10.1016/s0010-4655(02)00140-6

Cited by 44 publications

(42 citation statements)

References 24 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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“…In Table 6 we compare the present LS effective collision strengths with those of Sunderland et al (2002). Agreement between the two sets of data is good (within ∼20%), with the exception of the effective collision strengths for the 4 F− 2 D transition, which differs by ∼40%.…”

Section: Scattering Calculationsmentioning

confidence: 77%

“…Our target representation yields reasonably accurate energies, but the 2 H and 2 D terms come out in reverse energy order. By contrast, the target representation of Sunderland et al (2002) does predict the 2 H and 2 D terms in the correct order; yet their computed energies are considerably overestimated for all states of the 3d 7 configuration, perhaps due to missing configuration interaction.…”

Section: Scattering Calculationsmentioning

confidence: 90%

“…In the case of the 3d 6 4p configuration there are also problems because of the incomplete list of levels included, thus there maybe collisional coupling effects that are unaccounted for. The importance of including a large CC expansion, beyond the terms of the 3d 7 configuration, was demonstrated by Sunderland et al (2002). They showed that the collision strengths for transitions within the 3d 7 configuration were underestimated by up to 40% when the calculation neglected states of the 3d 6 4s and 3d 6 4p.…”

Section: Scattering Calculationsmentioning

confidence: 99%

“…radiative and collisional rates for Fe - (Bautista & Pradhan 1998), Ni  (Bautista 1999(Bautista , 2005, Ni  (Bautista 2001), and here we present a calculation for Ni . The first calculation of collisional data for Ni  was presented by Sunderland et al (2002), as a test case for a new parallel R-matrix program PRMAT. Nevertheless, this computation was wholly done in LS-coupling and is thus of limited practical use.…”

Section: Introductionmentioning

confidence: 99%

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Atomic data from the Iron project

Meléndez

Bautista

2005

A&A

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Abstract. This paper reports on radiative transition rates and electron impact excitation rate coefficients for levels of the 3d 7 ground configuration of Ni . The radiative data were computed using the Thomas-Fermi-Dirac central potential method, which allows for configuration interactions (CI) and relativistic effects in the Breit-Pauli formalism. Collision strengths in LS-coupling were calculated in the close coupling approximation with the R-matrix method. Then, fine structure collision strengths were obtained by means of the intermediate-coupling frame transformation (ICFT) method that accounts for spin-orbit coupling effects. The collision strengths were integrated over a Maxwellian distribution of electron energies, and the resulting effective collision strengths are given for a wide range of temperatures. We build a multilevel model for the Ni  system and use it to identify the most important lines in optical and infrared spectra and to compute line ratios as diagnostics of nebular conditions. Finally, we test these data against recent observations of the bipolar planetary nebula Mz 3.

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Introduction to Cluster Dynamics

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A parallel R-matrix program PRMAT for electron–atom and electron–ion scattering calculations

Cited by 44 publications

References 24 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 from the Iron project

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