Spectroscopic and photometric observations of SN 1987A – III. Days 135 to 260

Catchpole, R. M.; Menzies, John; Monk, A. S.; Wargau, W.; Pollaco, D.; Carter, B. S.; Whitelock, P. A.; Marang, F.; Laney, C. D.; Balona, L. A.; Feast, M. W.; Evans, T. H. H. Lloyd; Sekiguchi, K.; Laing, J. D.; Kilkenny, D.; Jones, J. H. Spencer; Roberts, G.; Cousins, A. W. J.; Vuuren, G. van; Winkler, Hartmut

doi:10.1093/mnras/231.1.75p

Cited by 97 publications

(33 citation statements)

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“…A value of ∆M = 2 M mimics hydrogen mixing down to zero velocity, which agrees with spectral observations, and produces the best match with the dome shape of SN 1987A. Catchpole et al (1987Catchpole et al ( , 1988, open circles) and Hamuy et al (1988, open triangles). For reference, Model 16-7b without the boxcar averaging of the chemical composition is shown with ∆M = 0 (magenta lines).…”

Section: Varying Explosion Parameterssupporting

confidence: 82%

Explosions of blue supergiants from binary mergers for SN 1987A

Menon

Utrobin

Heger

2018

Monthly Notices of the Royal Astronomical Society

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Based on the work of Menon and Heger (2017), we present the bolometric light curves and spectra of the explosions of blue supergiant progenitors from binary mergers. We study SN 1987A and two other peculiar Type IIP supernovae: SN 1998A and SN 2006V. The progenitor models were produced using the stellar evolution code Kepler and then exploded using the 1D radiation hydrodynamic code Crab. The explosions of binary merger models exhibit an overall better fit to the light curve of SN 1987A than previous single star models, because of their lower helium-core masses, larger envelope masses, and smaller radii. The merger model that best matches the observational constraints of the progenitor of SN 1987A and the light curve is a model with a radius of 37 R , an ejecta mass of 20.6 M , an explosion energy of 1.7 × 10 51 erg, a nickel mass of 0.073 M , and a nickel mixing velocity of 3,000 km s −1 . This model also works for SN 1998A and is comparable with earlier estimates from semi-analytic models. In the case of SN 2006V, however, a model with a radius of 150 R and ejecta mass of 19.1 M matches the light curve. These parameters are significantly higher than predictions from semi-analytic models for the progenitor of this supernova.

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Section: Varying Explosion Parameterssupporting

confidence: 82%

Explosions of blue supergiants from binary mergers for SN 1987A

Menon

Utrobin

Heger

2018

Monthly Notices of the Royal Astronomical Society

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“…The ejection of a small mass of 56 Ni provides a constraint on the mass of the collapsed -12remnant, M rem Thielemann et al 1996 Evans (private communication) have been also plotted. The insert shows the bolometric light curves of SN 1997D and SN 1987A (Catchpole et al 1987(Catchpole et al , 1988. The star marks the optical+IR spectrophotometric observation of Jan.30.…”

Section: Discussionmentioning

confidence: 99%

The Peculiar Type II Supernova 1997D: A Case for a Very Low [TSUP]56[/TSUP]N[CLC]i[/CLC] Mass

Turatto

Mazzali

Young

et al. 1998

The Astrophysical Journal

178

166

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SN 1997D in NGC 1536 is possibly the least luminous and energetic Type II supernova discovered to date. The entire light curve is subluminous, never reaching M V = −14.65. The radioactive tail follows the 56 Co decay slope. In the case of nearly complete trapping of the γ-rays, the 56 Ni mass derived from the tail brightness is extremely small, ∼ 0.002 M ⊙ . At discovery the spectra showed a red continuum and line velocities of the order of 1000 km s −1 . The luminosity and the photospheric expansion velocity suggest that the explosion occurred about 50 days before discovery, and that a plateau probably followed.Model light curves and spectra of the explosion of a 26 M ⊙ star successfully fit the observations. Low mass models are inconsistent with the observations. The radius of the progenitor, constrained by the prediscovery upper limits, islow explosion energy of ∼ 4 × 10 50 ergs is then required in the modeling. The strong Ba II lines in the photospheric spectra are reproduced with a solar abundance and low T eff . A scenario in which the low 56 Ni mass observed in SN 1997D is due to fall-back of material onto the collapsed remnant of the explosion of a 25-40 M ⊙ star appears to be favored over the case of the explosion of an 8-10 M ⊙ star with low 56 Ni production.

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“…CO emission in an erupting supernova was first seen (at ∼ 100 days after the explosion) in SN 1987A (Catchpole & Glass 1987;McGregor & Hyland 1987;Meikle et al 1989;Catchpole et al 1988;Olivia, Moorwood & Danziger 1987;Spyromilio et al 1988). The SiO fundamental at ∼ 8 µm was also observed, by Roche, Aitken & Smith (1993).…”

Section: Co and Dust Formation In Supernovaementioning

confidence: 99%

Early formation of carbon monoxide in the Centaurus A supernova SN 2016adj

Banerjee

Joshi

Evans

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present near-infrared spectroscopy of the NGC 5128 supernova SN 2016adj in the first 2 months following discovery. We report the detection of first overtone carbon monoxide emission at ∼ 58.2 d after discovery, one of the earliest detections of CO in an erupting supernova. We model the CO emission to derive the CO mass, temperature and velocity, assuming both pure 12 CO and a composition that includes 13 CO; the case for the latter is the isotopic analyses of meteoritic grains, which suggest that core collapse supernovae can synthesise significant amounts of 13 C. Our models show that, while the CO data are adequately explained by pure 12 CO, they do not preclude the presence of 13 CO, to a limit of 12 C/ 13 C> 3, the first constraint on the 12 C/ 13 C ratio determined from near-infrared observations. We estimate the reddening to the object, and the effective temperature from the energy distribution at outburst. We discuss whether the ejecta of SN 2016adj may be carbon-rich, what the infrared data tell us about the classification of this supernova, and what implications the early formation of CO in supernovae may have for CO formation in supernovae in general.

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Spectroscopic and photometric observations of SN 1987A – III. Days 135 to 260

Cited by 97 publications

References 0 publications

Explosions of blue supergiants from binary mergers for SN 1987A

Explosions of blue supergiants from binary mergers for SN 1987A

The Peculiar Type II Supernova 1997D: A Case for a Very Low [TSUP]56[/TSUP]N[CLC]i[/CLC] Mass

Early formation of carbon monoxide in the Centaurus A supernova SN 2016adj

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