THE SUPERLUMINOUS SN DES13S2cmm AS A SIGNATURE OF A QUARK-NOVA IN A HE-HMXB SYSTEM

Ouyed, Rachid; Leahy, D. A.; Koning, Nico

doi:10.1088/0004-637x/809/2/142

Cited by 6 publications

(5 citation statements)

References 35 publications

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“…2013hy SN 2013hy (=DES13S2cmm) was classified as a SLSN-I by Papadopoulos et al (2015) and as a "Gold" SLSN-I by Angus et al (2019). Ouyed et al (2015) argue SN 2013hy was actually a quark nova in a high mass X-ray binary. We only include photometry from Angus et al (2019).…”

Section: B3 2007cementioning

confidence: 99%

Luminous Supernovae: Unveiling a Population Between Superluminous and Normal Core-collapse Supernovae

Gómez¹,

Berger²,

Nicholl³

et al. 2022

Preprint

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Stripped-envelope core-collapse supernovae can be divided into two broad classes: the common Type Ib/c supernovae (SNe Ib/c), powered by the radioactive decay of 56 Ni, and the rare superluminous supernovae (SLSNe), most likely powered by the spin-down of a magnetar central engine. Up to now, the intermediate regime between these two populations has remained mostly unexplored. Here, we present a comprehensive study of 40 luminous supernovae (LSNe), SNe with peak magnitudes of M r = −19 to −20 mag, bound by SLSNe on the bright end and by SNe Ib/c on the dim end. Spectroscopically, LSNe appear to form a continuum between Type Ic SNe and SLSNe. Given their intermediate nature, we model the light curves of all LSNe using a combined magnetar plus radioactive decay model and find that they are indeed intermediate, not only in terms of their peak luminosity and spectra, but also in their rise times, power sources, and physical parameters. We sub-classify LSNe into distinct groups that are either as fast-evolving as SNe Ib/c or as slow-evolving as SLSNe, and appear to be either radioactively or magnetar powered, respectively. Our findings indicate that LSNe are powered by either an over-abundant production of 56 Ni or by weak magnetar engines, and may serve as the missing link between the two populations.

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Section: B3 2007cementioning

confidence: 99%

Luminous Supernovae: Unveiling a Population Between Superluminous and Normal Core-collapse Supernovae

Gómez¹,

Berger²,

Nicholl³

et al. 2022

Preprint

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“…The computation of the QN light curve is given in Appendix in Ouyed et al (2015b) where the He-rich CE initial shock temperature (T CE,0 ; following impact by the QN ejecta) was estimated from the shocked gas pressure.…”

Section: The Qn Phasementioning

confidence: 99%

“…second) CE (M He ) and its initial radius R CE,0 . The evolution of the CE radius is then R CE = R CE,0 + v QN (t − t BO ) where t BO is the time of QN shock breakout; see Appendix in Ouyed et al (2015b) on the time evolution of the CE radius, its temperature, the photosphere and the calculation of the QN light curve.…”

Section: The Qn Phasementioning

confidence: 99%

Quark-Novae Occurring in Massive Binaries: A Universal Energy Source in Superluminous Supernovae With Double-Peaked Light Curves

Ouyed¹,

Leahy²,

Koning

2016

ApJ

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A Quark-Nova (QN; the sudden transition from a neutron star into a quark star) which occurs in the second common envelope (CE) phase of a massive binary (Ouyed et al., 2015a&b), gives excellent fits to super-luminous, hydrogen-poor, Supernovae (SLSNe) with double-peaked light curves including DES13S2cmm, SN 2006oz and LSQ14bdq (http://www.quarknova.ca/LCGallery.html). In our model, the H envelope of the less massive companion is ejected during the first CE phase while the QN occurs deep inside the second, He-rich, CE phase after the CE has expanded in size to a radius of a few tens to a few thousands solar radii; this yields the first peak in our model. The ensuing merging of the quark star with the CO core leads to black hole formation and accretion explaining the second long-lasting peak. We study a sample of 8 SLSNe Ic with double-humped light-curves. Our model provides good fits to all of these with a universal explosive energy of 2 × 10 52 erg (which is the kinetic energy of the QN ejecta) for the first hump. The late-time emissions seen in iPTF13ehe and LSQ14bdq are fit with a shock interaction between the outgoing He-rich (i.e second) CE and the previously ejected H-rich (i.e first) CE.

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“…and undergoes a QN explosion inside the expanded Hydrogen-poor envelope. The QN ejecta shocks and unbinds the CE providing a bright, short-lived hump matching those observed in double-humped SLSNe 29,30 .…”

Section: Quark Novae In Massive Binaries : a Model For Slsne Iamentioning

confidence: 56%

“…. In particular, in massive binaries experiencing two CE phases, the NS would have access to two mass reservoirs 29,30 . In this picture, the NS would have evolved earlier from its more massive progenitor and is companion to the second star during its CE phase.…”

Section: Quark Novae In Massive Binaries : a Model For Slsne Iamentioning

confidence: 99%

Quark-novae in binaries: Observational signatures and implications to astrophysics

Ouyed¹,

Leahy²,

Koning³

et al. 2017

The Fourteenth Marcel Grossmann Meeting

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The explosive transition of a massive neutron star to a quark star (the Quark-Nova; QN) releases in excess of ∼ 10 52 erg in kinetic energy which can drastically impact the surrounding environment of the QN. A QN is triggered when a neutron star gains enough mass to reach the critical value for quark deconfinement to happen in the core. In binaries, a neutron star has access to mass reservoirs (e.g. accretion from a companion or from a Common Envelope; CE). We explain observed light-curves of hydrogen-poor superluminous Supernovae (SLSNe Ia) in the context of a QN occurring in the second CE phase of a massive binary. In particular this model gives good fits to light-curves of SLSNe with double-humped light-curves. Our model suggests the QN as a mechanism for CE ejection and that they be taken into account during binary evolution. In a short period binary with a white dwarf companion, the neutron star can quickly grow in mass and experience a QN event. Part of the QN ejecta collides with the white dwarf; shocking, compressing; and heating it to driving a thermonuclear runaway producing a SN Ia impostor (a QN-Ia). Unlike "normal" Type Ia supernovae where no compact remnant is formed, a QN-Ia produces a quark star undergoing rapid spin-down providing additional power along with the 56 Ni decay energy. Type Ia SNe are used as standard candles and contamination of this data by QNe-Ia can infer an incorrect cosmology.

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THE SUPERLUMINOUS SN DES13S2cmm AS A SIGNATURE OF A QUARK-NOVA IN A HE-HMXB SYSTEM

Cited by 6 publications

References 35 publications

Luminous Supernovae: Unveiling a Population Between Superluminous and Normal Core-collapse Supernovae

Luminous Supernovae: Unveiling a Population Between Superluminous and Normal Core-collapse Supernovae

Quark-Novae Occurring in Massive Binaries: A Universal Energy Source in Superluminous Supernovae With Double-Peaked Light Curves

Quark-novae in binaries: Observational signatures and implications to astrophysics

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