SN 2006aj Associated with XRF 060218 at Late Phases: Nucleosynthesis Signature of a Neutron Star-driven Explosion

Maeda, Keiichi; Kawabata, Koji S.; Tanaka, Masaomi; Nomoto, Ken’ichi; Tominaga, Nozomu; Hattori, Takashi; Minezaki, Takeo; Kuroda, T.; Suzuki, Tomoharu; Deng, J. S.; Mazzali, P. A.; Pian, E.

doi:10.1086/513564

Cited by 87 publications

(103 citation statements)

References 30 publications

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“…A detection of [Ni II] λ7378 was reported also for the broad-lined Type Ic SN 2006aj (Maeda et al 2007;Mazzali et al 2007) which was associated with an X-ray flash (Mazzali et al 2006). The [Ni II] identification was somewhat hampered by high noise levels combined with very large widths of the emission lines.…”

Section: Discussion and Summarymentioning

confidence: 86%

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: 86%

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 fact, it has been often proposed that such GRBs, only observed at smaller redshift 0.0085 < z < 0.168, form a different class, less luminous and possibly much more numerous than the high luminosity GRBs at higher redshift (Pian et al, 2006;Soderberg et al, 2004;Maeda et al, 2007;. Therefore in the current literature they have been proposed to originate from a separate class of progenitors Cobb et al, 2006).…”

Section: The "Fireshell" Model and Grb Progenitorsmentioning

confidence: 98%

GRB060614: a “fake” short GRB from a merging binary system

Caito

Bernardini

Bianco

et al. 2009

A&A

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Context. GRB060614 observations by VLT and by Swift have infringed the traditionally accepted gamma-ray burst (GRB) collapsar scenario that purports the origin of all long duration GRBs from supernovae (SN). GRB060614 is the first nearby long duration GRB clearly not associated with a bright Ib/c SN. Moreover, its duration (T 90 ∼ 100 s) makes it hardly classifiable as a short GRB. It presents strong similarities with GRB970228, the prototype of a new class of "fake" short GRBs that appear to originate from the coalescence of binary neutron stars or white dwarfs spiraled out into the galactic halo. Aims. Within the "canonical" GRB scenario based on the "fireshell" model, we test if GRB060614 can be a "fake" or "disguised" short GRB. We model the traditionally termed "prompt emission" and discriminate the signal originating from the gravitational collapse leading to the GRB from the process occurring in the circumburst medium (CBM). Methods. We fit GRB060614 light curves in Swift's BAT (15 − 150 keV) and XRT (0.2 − 10 keV) energy bands. Within the fireshell model, light curves are formed by two well defined and different components: the proper-GRB (P-GRB), emitted when the fireshell becomes transparent, and the extended afterglow, due to the interaction between the leftover accelerated baryonic and leptonic shell and the CBM. Results. We determine the two free parameters describing the GRB source within the fireshell model: the total e ± plasma energy (E e ± tot = 2.94 × 10 51 erg) and baryon loading (B = 2.8 × 10 −3 ). A small average CBM density ∼ 10 −3 particles/cm 3 is inferred, typical of galactic halos. The first spikelike emission is identified with the P-GRB and the following prolonged emission with the extended afterglow peak. We obtain very good agreement in the BAT (15 − 150 keV) energy band, in what is traditionally called "prompt emission", and in the XRT (0.2 − 10 keV) one. Conclusions. The anomalous GRB060614 finds a natural interpretation within our canonical GRB scenario: it is a "disguised" short GRB. The total time-integrated extended afterglow luminosity is greater than the P-GRB one, but its peak luminosity is smaller since it is deflated by the peculiarly low average CBM density of galactic halos. This result points to an old binary system, likely formed by a white dwarf and a neutron star, as the progenitor of GRB060614 and well justifies the absence of an associated SN Ib/c. Particularly important for further studies of the final merging process are the temporal structures in the P-GRB down to 0.1 s.

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“…The SN is assumed to lead to the formation of a neutron star (NS) or to a complete disruptive explosion without remnants and, in no way, to the formation of a black hole. In the case of SN2006aj the formation of such a NS has been inferred by Maeda et al (2007) because of the large amount of 58 Ni (0.05 M ). Moreover the significantly small initial mass of the SN progenitor star M ≈ 20 M is expected to form a NS rather than a black hole when its core collapses (Maeda et al 2007;Ferrero et al 2006;Mazzali et al 2006;Nomoto et al 2007).…”

Section: Binaries As Progenitors Of Grb-sn Systemsmentioning

confidence: 99%

“…In the case of SN2006aj the formation of such a NS has been inferred by Maeda et al (2007) because of the large amount of 58 Ni (0.05 M ). Moreover the significantly small initial mass of the SN progenitor star M ≈ 20 M is expected to form a NS rather than a black hole when its core collapses (Maeda et al 2007;Ferrero et al 2006;Mazzali et al 2006;Nomoto et al 2007). In order to fulfill both the above requirement, we assume that the progenitor of the GRB and the SN consists of a binary system formed by a NS close to its critical mass collapsing to a black hole, and a companion star evolved out of the main sequence originating the SN.…”

Section: Binaries As Progenitors Of Grb-sn Systemsmentioning

confidence: 99%

“…It has been often proposed that GRBs associated with SNe Ib/c, at smaller redshift 0.0085 < z < 0.168 (e.g. , and references therein), form a different class, less luminous and possibly much more numerous than the high luminosity GRBs at higher redshift Soderberg et al 2004;Maeda et al 2007;. Therefore they have been proposed to originate from a separate class of progenitors (Liang et al 2006b;Cobb et al 2006).…”

Section: Binaries As Progenitors Of Grb-sn Systemsmentioning

confidence: 99%

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GRB 060218 and GRBs associated with supernovae Ib/c

Dainotti¹,

Bernardini²,

Bianco³

et al. 2007

A&A

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Context. The Swift satellite has given continuous data in the range 0.3-150 keV from 0 s to 10 6 s for GRB 060218 associated with SN2006aj. This Gamma-Ray Burst (GRB) which has an unusually long duration (T 90 ∼ 2100 s) fulfills the Amati relation. These data offer the opportunity to probe theoretical models for GRBs connected with Supernovae (SNe). Aims. We plan to fit the complete γ-and X-ray light curves of this long duration GRB, including the prompt emission, in order to clarify the nature of the progenitors and the astrophysical scenario of the class of GRBs associated with SNe Ib/c. Methods. We apply our "fireshell" model based on the formation of a black hole, giving the relevant references. It is characterized by the precise equations of motion and equitemporal surfaces and by the role of thermal emission. Results. The initial total energy of the electron-positron plasma E tot e ± = 2.32 × 10 50 erg has a particularly low value, similar to the other GRBs associated with SNe. For the first time, we observe a baryon loading B = 10 −2 which coincides with the upper limit for the dynamical stability of the fireshell. The effective CircumBurst Medium (CBM) density shows a radial dependence n cbm ∝ r −α with 1.0 < ∼ α < ∼ 1.7 and monotonically decreases from 1 to 10 −6 particles/cm 3 . This behavior is interpreted as being due to a fragmentation in the fireshell. Analogies with the fragmented density and filling factor characterizing Novae are outlined. The fit presented is particularly significant in view of the complete data set available for GRB 060218 and of the fact that it fulfills the Amati relation. Conclusions. We fit GRB 060218, usually considered as an X-Ray Flash (XRF), as a "canonical GRB" within our theoretical model. The smallest possible black hole, formed by the gravitational collapse of a neutron star in a binary system, is consistent with the especially low energetics of the class of GRBs associated with SNe Ib/c. We provide the first evidence for a fragmentation in the fireshell. This fragmentation is crucial in explaining both the unusually large T 90 and the consequently inferred abnormally low value of the CBM effective density.

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SN 2006aj Associated with XRF 060218 at Late Phases: Nucleosynthesis Signature of a Neutron Star-driven Explosion

Cited by 87 publications

References 30 publications

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

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

GRB060614: a “fake” short GRB from a merging binary system

GRB 060218 and GRBs associated with supernovae Ib/c

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