Nickel, argon and cobalt in the infrared spectrum of SN1987A: the core becomes visible

Rank, D. M.; Pinto, Philip A.; Woosley, S. E.; Bregman, J. D.; Wittebornt, F. C.; Axelrod, T. S.; Cohen, Martin

doi:10.1038/331505a0

Cited by 61 publications

(29 citation statements)

References 3 publications

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“…Regarding ionization, we find about 80% of the nickel being singly ionized between 250 and 450 days, with most of the remainder being Ni III. The most questionable assumption in the Rank et al (1988) and Wooden et al (1993) derivation is that of optically thin emission; in our models the [Ni II] 6.636 µm line has an optical depth of 3.2 at 250 days and 1.5 at 450 days. This optical depth leads to an underestimate of the Ni mass by a factor of 2-3 if one uses the optically thin formula.…”

Section: Discussion and Summarymentioning

confidence: 97%

“…Asplund et al (2009) Estimates of the Ni/Fe ratio has been presented (to our knowledge) for four previous core-collapse SNe. For SN 1987A, Rank et al (1988) reported a measurement of the [Ni II] 6.636 µm luminosity at 262 days. Assuming LTE, optically thin conditions, and that most nickel is singly ionized, this luminosity gave a Ni mass of 2 × 10 −3 M⊙, which with M (Fe) = 0.075 M⊙ from the 56 Ni measurement gives Ni/Fe = 0.027, less than half the solar value.…”

Section: Discussion and Summarymentioning

confidence: 99%

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Supersolar Ni/Fe production in the Type IIP SN 2012ec

Jerkstrand

Smartt

Sollerman

et al. 2015

Monthly Notices of the Royal Astronomical Society

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SN 2012ec is a Type IIP supernova (SN) with a progenitor detection and comprehensive photospheric-phase observational coverage. Here, we present Very Large Telescope and PESSTO observations of this SN in the nebular phase. We model the nebular [O I] λλ6300, 6364 lines and find their strength to suggest a progenitor main-sequence mass of 13 − 15 M ⊙ . SN 2012ec is unique among hydrogen-rich SNe in showing a distinct line of stable nickel [Ni II] λ7378. This line is produced by 58 Ni, a nuclear burning ash whose abundance is a sensitive tracer of explosive burning conditions. Using spectral synthesis modelling, we use the relative strengths of [Ni II] λ7378 and [Fe II] λ7155 (the progenitor of which is 56 Ni) to derive a Ni/Fe production ratio of 0.20 ± 0.07 (by mass), which is a factor 3.4 ± 1.2 times the solar value. High production of stable nickel is confirmed by a strong [Ni II] 1.939 µm line. This is the third reported case of a core-collapse supernova producing a Ni/Fe ratio far above the solar value, which has implications for core-collapse explosion theory and galactic chemical evolution models.

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Section: Discussion and Summarymentioning

confidence: 97%

Section: Discussion and Summarymentioning

confidence: 99%

Supersolar Ni/Fe production in the Type IIP SN 2012ec

Jerkstrand

Smartt

Sollerman

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…In 1987 molecular emission from a SN was detected for the first time in the type I1 object SN1987a [47,48]. The emissions originate from vibrational bands of CO, SiO, and possibly CS [49].…”

Section: Type I1 Supernovaementioning

confidence: 97%

Heavy particle atomic collisions in astrophysics: Beyond H and He targets

Stancil¹,

Krstic²,

Schultz³

1998

Atomic Processes in Plasmas

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Abstract. The physical conditions relatini to the emission of x-rays from Jovi Rec El v E 0 HAY I 4 ' 1998 QWd and cometary atmospheres and to supernova ejecta are briefly described. Emphasis is placed on elucidating the relevance and importance of atomic collision processes, the availability of data, and the outstanding data needs for modeling these environments. Some preliminary theoretical studies of electron capture for important collisions systems, involving molecular and atomic metal targets, are presented.

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“…The most obvious feature of Figure 1 is the disparate behavior of the M light curve. This has now been conclusively shown to be due to emission in the fundamental bands of CO (McGregor and Hyland 1987;Oliva, Moorwood and Danziger 1987;Rank et al 1988b;Catchpole et al 1988;Bouchet et al 1988). The timescale for decline of the M light curve after day 230 agrees well with the 5 6 Co mean lifetime, suggesting that the fundamental band CO emission is closely tied to the bolometric luminosity.…”

mentioning

confidence: 92%

“…The identified lines are due to neutral and singly ionized species with ionization potentials less than ~ 16 eV, broadly consistent with thermal excitation at a temperature near the photospheric temperature. Rank et al (1988b) have noted that model calculations predict a low excitation spectrum due to the high envelope density and efficient cooling by metals. A curious feature of the near-infrared spectrum is a redshift of all identified emission lines by 400-1500 km s _ 1 with respect to the LMC (Oliva, Moorwood and Danziger 1987).…”

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confidence: 99%

Observations of SN 1987A in the Near-infrared

McGregor

1988

Publ. Astron. Soc. Aust.

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High quality near-infrared (1-5 /jm) spectra of SN 1987A have been obtained at MSSSO, AAO, ESO, CTIO and SAAO with good temporal coverage. These near-infrared observations are reviewed with particular reference to spectra obtained by the MSSSO group on the ANU 2.3m telescope at Siding Spring Observatory. I n t r o d u c t i o nSN 1987A continues to be extensively monitored both photometrically and spectroscopically in the nearinfrared. These d a t a are of high quality with good temporal coverage and should be incorporated in detailed supernova models. The near-infrared spectra now available to the comumunity complement optical spectra and offer advantages of large numbers of relatively unblended lines and accurate continuum flux densities, as well as information on species which are not represented in the optical region. In particular, near-infrared hydrogen line profiles have indicated the minimum velocity of the hydrogen shell, the presence of He I absorption gives information on the 7-ray flux, and the detection in SN 1987A of CO first-overtone band head emission represents the first detection of molecules in a supernova. The aim of this review is to present some of the data on SN 1987A being obtained in the 1-5 fim region and to discuss model constraints that have been derived from initial analyses of these data.

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Nickel, argon and cobalt in the infrared spectrum of SN1987A: the core becomes visible

Cited by 61 publications

References 3 publications

Supersolar Ni/Fe production in the Type IIP SN 2012ec

Supersolar Ni/Fe production in the Type IIP SN 2012ec

Heavy particle atomic collisions in astrophysics: Beyond H and He targets

Observations of SN 1987A in the Near-infrared

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