Optical and infrared observations of radioactive elements in supernovae

Sollerman, J.

doi:10.1016/s1387-6473(02)00189-6

Cited by 17 publications

(15 citation statements)

References 21 publications

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“…Thus, all SNe II from stars with M > 10 M ⊙ could be SNe II(L). This removes the conflict between our earlier model and observations of SN II light curves, which showed that most SNe II produce ∼ 0.1 M ⊙ of Fe (e.g., Table 1 in Sollerman 2002). With this Fe yield and a Galactic SN II rate of ∼ (30 yr) −1 , ∼ 3 × 10 8 SNe II over the Galactic history of ∼ 10 10 yr would enrich the total baryonic mass of ∼ 10 11 M ⊙ in the Galaxy with ∼ 1/3 of the solar Fe mass fraction (≈ 10 −3 ).…”

Section: Discussionmentioning

confidence: 71%

Stellar Sources for Heavyr‐Process Nuclei

Qian

Wasserburg

2003

ApJ

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The stellar sites and the complete mechanism of r-process nucleosynthesis are still unresolved issues. From consideration of the observed abundances in metal-poor stars, it is proposed that the production of the heavy r-process nuclei (r-nuclei with mass numbers A > 130) is not related to the production of the Fe group elements or of the elements with lower atomic numbers: Na, Mg, Al, Si, Ca, Sc, and Ti. This requires that the production of the heavy r-nuclei not occur in supernovae with extended shell structure, but be associated with either bare neutron stars or Type II supernovae (SNe II) in the mass range 8 M ⊙ < M < 10 M ⊙ . From the observations of stars with [Fe/H] ∼ −3 but with high abundances of r-elements, it is clear that these r-process enrichments cannot represent the composition of the interstellar medium from which the stars were formed, but must represent very local contamination from binary companions. Further evidence for very high enrichments of s-process elements in metal-poor stars also requires binary systems for explanation. We propose that the accretion-induced collapse (AIC) of a white dwarf into a neutron star in a binary system may be associated with the production of the heavy r-nuclei and may provide occasional coupling of high r-process and high s-process enrichments in the envelopes of low-mass stars with low [Fe/H]. If we assume that the bulk of the heavy r-nuclei are produced in AIC events, then these events would have produced ∼ 1.6 × 10 9 neutron stars in the Galaxy. A much larger number of white dwarf binaries would have resulted from the evolution of other binary systems. The AIC scenario removes the assignment in our earlier model that SNe II provide the bulk of the heavy r-nuclei and relegates r-process production in SNe II to the light r-nuclei with A 130. This new assignment removes the requirement in our earlier model that most SNe II produce no Fe and gives Fe yields that are in accord with the observed values for most SNe II.

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Section: Discussionmentioning

confidence: 71%

Stellar Sources for Heavyr‐Process Nuclei

Qian

Wasserburg

2003

ApJ

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“…Thus, we conclude conservatively that the 56 Ni mass of SN 2011ht lies in the range of 0.006-0.01 M⊙. Despite the large uncertainty, we can state with confidence that the range of likely values for the 56 Ni mass occupies the low end of the range exhibited by SNe II-P (Turatto et al 1990;Sollerman 2002;Nadyozhin 2003;Smartt et al 2009), which has important implications that will be discussed below.…”

Section: Low 56 Ni Massmentioning

confidence: 73%

SN 2011ht: confirming a class of interacting supernovae with plateau light curves (Type IIn-P)

Mauerhan

Smith

Silverman

et al. 2013

Monthly Notices of the Royal Astronomical Society

104

111

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We present photometry and spectroscopy of the Type IIn supernova (SN) 2011ht, identified previously as a possible SN impostor. The light curve exhibits an abrupt transition from a well-defined ∼ 120 day plateau to a steep bolometric decline, plummeting 4-5 mag in the optical and 2-3 mag in the infrared in only ∼ 10 days. Leading up to peak brightness (M V = −17.4 mag), a hot emission-line spectrum exhibits strong signs of interaction with circumstellar material (CSM), in the form of relatively narrow P-Cygni features of H i and He i superimposed on broad Lorentzian wings. For the latter half of the plateau phase, the spectrum exhibits strengthening P-Cygni profiles of Fe ii, Ca ii, and Hα. By day 147, after the plateau has ended, the SN entered the nebular phase, heralded by the appearance of forbidden transitions of [O i], [O ii], and [Ca ii] over a weak continuum. At this stage, the light curve exhibits a low optical luminosity that is comparable to that of the most subluminous Type II-P supernovae, and a relatively fast visual wavelength decline that appeared to be significantly steeper than the 56 Co decay rate. However, the total pseudo-bolometric decline, including the infrared luminosity, is consistent with 56 Co decay, and implies a low 56 Ni mass in the range 0.006-0.01 M ⊙ , near the lower end of the range exhibited by SNe II-P. We therefore characterize SN 2011ht as a core-collapse SN very similar to the peculiar SNe IIn 1994W and 2009kn. These three SNe appear to define a subclass, which are Type IIn based on their spectrum, but that also exhibit well-defined plateaus and produce low 56 Ni yields. We therefore suggest Type IIn-P as a name for this subclass. The absence of observational signatures of high-velocity material from SNe IIn-P could be the result of an opaque shell at the shocked SN-CSM interface, which remains optically thick longer than the time scale for the inner ejecta to cool and become transparent. Possible progenitors of SNe IIn-P, consistent with the available data, include 8-10 M ⊙ stars, which undergo core collapse as a result of electron capture after a brief phase of enhanced mass loss, or more massive (M 25 M ⊙ ) progenitors, which experience substantial fallback of the metal-rich radioactive ejecta. In either case, the energy radiated by these three SNe during their plateau (2-3 × 10 49 erg for SN 2011ht) must be dominated by CSM interaction, and the subluminous tail the result of low 56 Ni yield.

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“…After this plateau or photospheric phase, the bolometric light curve shows a rapid decay followed by a transition to a linear decline of ∼ 0.98 magnitudes every 100 days (e.g. Sollerman 2002). During this post-explosion period (radioactive-decay phase), the continuum electromag-⋆ E-mail: mlpumo@astropa.unipa.it or mlpumo@oact.inaf.it netic emission is thought to be powered by the energy released from the radioactive decay of 56 Ni through the nuclear decay chain 56 Ni → 56 Co → 56 Fe (e.g.…”

Section: Introductionmentioning

confidence: 99%

Radiation-hydrodynamical modelling of underluminous Type II plateau supernovae

Pumo

Zampieri

Spiro

et al. 2016

Mon. Not. R. Astron. Soc.

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With the aim of improving our knowledge about the nature of the progenitors of low-luminosity Type II plateau supernovae (LL SNe IIP), we made radiationhydrodynamical models of the well-sampled LL SNe IIP 2003Z, 2008bk and 2009md. For these three SNe we infer explosion energies of 0.16-0.18 foe, radii at explosion of 1.8-3.5 × 10 13 cm, and ejected masses of 10-11.3M ⊙ . The estimated progenitor mass on the main sequence is in the range ∼ 13.2-15.1M ⊙ for SN 2003Z and ∼ 11.4-12.9M ⊙ for SNe 2008bk and 2009md, in agreement with estimates from observations of the progenitors. These results together with those for other LL SNe IIP modelled in the same way, enable us also to conduct a comparative study on this SN sub-group. The results suggest that: a) the progenitors of faint SNe IIP are slightly less massive and have less energetic explosions than those of intermediate-luminosity SNe IIP; b) both faint and intermediate-luminosity SNe IIP originate from low-energy explosions of red (or yellow) supergiant stars of low-to-intermediate mass; c) some faint objects may also be explained as electron-capture SNe from massive super-asymptotic giant branch stars; and d) LL SNe IIP form the underluminous tail of the SNe IIP family, where the main parameter "guiding" the distribution seems to be the ratio of the total explosion energy to the ejected mass. Further hydrodynamical studies should be performed and compared to a more extended sample of LL SNe IIP before drawing any conclusion on the relevance of fall-back to this class of events.

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Optical and infrared observations of radioactive elements in supernovae

Cited by 17 publications

References 21 publications

Stellar Sources for Heavyr‐Process Nuclei

Stellar Sources for Heavyr‐Process Nuclei

SN 2011ht: confirming a class of interacting supernovae with plateau light curves (Type IIn-P)

Radiation-hydrodynamical modelling of underluminous Type II plateau supernovae

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