SN 1992A: Ultraviolet and Optical Studies Based on HST, IUE, and CTIO Observations

Kirshner, R.; Jeffery, David J.; Leibundgut, B.; Challis, P.; Sonneborn, G.; Phillips, M. M.; Suntzeff, Nicholas B.; Smith, R. C.; Winkler, P. F.; Winge, Cláudia; Hamuy, M.; Hunter, Deidre A.; Roth, Katherine C.; Blades, J. C.; Branch, David; Chevalier, Roger A.; Fransson, Claes; Panagia, N.; Wagoner, Robert V.; Wheeler, J. C.; Harkness, Robert

doi:10.1086/173188

Cited by 190 publications

(180 citation statements)

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“…Figure A1: Comparison of the solar flux distribution (thin line, Kohl, Parkinson & Kurucz 1992, Neckel & Labs 1984, Labs & Neckel 1970, White 1977, Avrett 1992 with the observations of SN1992A at about 5 days past maximum light (thick line, Kirshner et al 1993). Both spectra are normalized to the bolometric irradiance of the sun measured in µW/cm 2 /nm.…”

Section: Appendix: Remark On Bolometric Correctionsmentioning

confidence: 99%

Explosion Models for Type IA Supernovae: A Comparison with Observed Light Curves, Distances, H 0, and Q 0

Hoêflich¹,

Khokkhlov²

1996

ApJ

471

538

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Theoretical monochromatic light curves and photospheric expansion velocities are compared with observations of 27 Type Ia supernovae (SNe Ia). A set of 37 models has been considered which encompasses all currently discussed explosion scenarios for Type Ia supernovae including deflagrations, detonations, delayed detonations, pulsating delayed detonations and tamped detonations of Chandrasekhar mass, and Helium detonations of low mass white dwarfs. The explosions are calculated using one-dimensional Lagrangian hydro and radiation-hydro codes with incorporated nuclear networks. Subsequently, light curves are constructed using our LC scheme which includes an implicit radiation transport, expansion opacities, a Monte-Carlo γ-ray transport, and molecular and dust formation. For some supernovae, results of detailed non-LTE calculations have been considered.Observational properties of our series of models are discussed, in particular, the relation between the absolute brightness, post-maximum decline rates, the colors at several moments of time, etc. All models with a 56 Ni production larger than ≈ 0.4M ⊙ produce light curves of similar brightness. The influence of the cosmological red shift on the light curves and on the correction for interstellar reddening is discussed.Based on data rectification of the standard deviation, a quantitative procedure to fit the observations has been used to the determine the free parameters, i.e. the distance, the reddening, and the time of the explosion. Fast rising light curves (e.g., SN 1981B and SN 1994D) can be reproduced by delayed detonation models or deflagration models similar to W7. Slowly rising (t max ≥ 16 days) light curves (e.g., SN 1984A and SN 1990N) cannot be reproduced by standard detonation, deflagration, or delayed detonation models. To obtain an acceptable agreement with observations, models are required where the C/O white dwarf is surrounded by an unburnt extended envelope of typically 0.2 to 0.4 M ⊙ which may either be pre-existing or produced during the explosion. Our interpretation of the light curves is also supported by the photospheric expansion velocities. Mainly due to the fast increase of the γ radiation produced by the outer 56 Ni , the post maximum decline of Helium detonations tends to be faster compared to observations of normal bright SNe Ia.Strongly subluminous SNe Ia can be understood in the framework of pulsating delayed detonations, both from the absolute brightness and the colors. Alternatively, subluminosity can be produced within the scenario of helium detonations in low mass white dwarfs of about 0.6 to 0.8 M ⊙ if the explosion occurs when rather little Helium has been accreted. However, even subluminous Helium detonation models are very blue at maximum light owing to heating in the outer layers and brighter models show a fast postmaximum decline, in contradiction to the observations. 3We find evidence for a correlation between the type of host galaxy and the explosion mechanism. In spiral galaxies, about the same amount of prompt exp...

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Section: Appendix: Remark On Bolometric Correctionsmentioning

confidence: 99%

Explosion Models for Type IA Supernovae: A Comparison with Observed Light Curves, Distances, H 0, and Q 0

Hoêflich¹,

Khokkhlov²

1996

ApJ

471

538

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show abstract

“…Features at longer wavelength (i.e., 2800 Å) are formed well within the SN ejecta and are products of nuclear burning (e.g., Branch & Venkatakrishna 1986;Kirshner et al 1993;Sauer et al 2008). Conspicuous features in this region are those around 3000 Å and 3250 Å, which are blends of Fe II or Co II (e.g., Branch & Venkatakrishna 1986).…”

Section: The 3000 å Featurementioning

confidence: 99%

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv

Gall

Stritzinger

Ashall

et al. 2018

A&A

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We present an analysis of ultraviolet (UV) to near-infrared observations of the fast-declining Type Ia supernovae (SNe Ia) 2007on and 2011iv, hosted by the Fornax cluster member NGC 1404. The B-band light curves of SN 2007on and SN 2011iv are characterised by ∆m 15 (B) decline-rate values of 1.96 mag and 1.77 mag, respectively. Although they have similar decline rates, their peak B-and H-band magnitudes differ by ∼ 0.60 mag and ∼ 0.35 mag, respectively. After correcting for the luminosity vs. decline rate and the luminosity vs. colour relations, the peak B-band and H-band light curves provide distances that differ by ∼ 14% and ∼ 9%, respectively. These findings serve as a cautionary tale for the use of transitional SNe Ia located in early-type hosts in the quest to measure cosmological parameters. Interestingly, even though SN 2011iv is brighter and bluer at early times, by three weeks past maximum and extending over several months, its B − V colour is 0.12 mag redder than that of SN 2007on. To reconcile this unusual behaviour, we turn to guidance from a suite of spherical one-dimensional Chandrasekhar-mass delayed-detonation explosion models. In this context, 56 Ni production depends on both the so-called transition density and the central density of the progenitor white dwarf. To first order, the transition density drives the luminosity-width relation, while the central density is an important second-order parameter. Within this context, the differences in the B − V color evolution along the Lira regime suggests the progenitor of SN 2011iv had a higher central density than SN 2007on.

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“…The composition of a delayeddetonation model is plotted against velocity in Figure 17 of Nomoto et al (1994) and that of model DD4 of Woosley & Weaver is displayed in Figure 4 of Kirshner et al (1993). Both models have a carbon-rich zone above 125,000 km s Ϫ1 , atop a region of oxygen and synthesized intermediate-mass elements.…”

Section: Implications For Explosion Modelsmentioning

confidence: 99%

Evidence for a High-Velocity Carbon-rich Layer in the Type I[CLC]a[/CLC] SN 1990N

Fisher

Branch

Nugent

et al. 1997

The Astrophysical Journal

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102

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We use a parameterized spectrum-synthesis code to make a direct analysis of a high quality spectrum of the Type Ia SN 1990N that was obtained by Leibundgut et al. 14 days before the time of optical maximum. We suggest that the absorption feature observed near 6040 Å, which has been attributed to blueshifted 6355 of Si II, actually was produced by blueshifted 6580 of C II, in a high-velocity (v Ͼ 26, 000 km s Ϫ1 ) carbon-rich region. Implications for SN Ia explosion models are briefly discussed.

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SN 1992A: Ultraviolet and Optical Studies Based on HST, IUE, and CTIO Observations

Cited by 190 publications

References 0 publications

Explosion Models for Type IA Supernovae: A Comparison with Observed Light Curves, Distances, H 0, and Q 0

Explosion Models for Type IA Supernovae: A Comparison with Observed Light Curves, Distances, H 0, and Q 0

Two transitional type Ia supernovae located in the Fornax cluster member NGC 1404: SN 2007on and SN 2011iv

Evidence for a High-Velocity Carbon-rich Layer in the Type I[CLC]a[/CLC] SN 1990N

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