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Post Info TOPIC: Gaia16apd
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RE: Gaia16apd
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Title: The magnetar model of the superluminous supernova GAIA16apd and the explosion jet feedback mechanism (JFM)
Author: Noam Soker (Technion, Israel)

Under the assumption that jets explode core collapse supernovae in a negative jet feedback mechanism (JFM), I show that rapidly rotating neutron stars are likely to be formed when the explosion is very energetic. Under the assumption that an accretion disk or an accretion belt around the just-formed neutron star launch jets and that the accreted gas spins-up the just-formed neutron star, I derive a crude relation between the energy that is stored in the spinning neutron star and the explosion energy. This relation reads Espin/Eexp~(Eexp/1e52erg). It shows that within the frame of the JFM explosion model of core collapse supernovae, spinning neutron stars, such as magnetars, might have significant energy in super-energetic explosions. The existence of magnetars, if confirmed, such as in the recent super-energetic supernova GAIA16apd, further supports my call for a paradigm shift from neutrino-driven to jet-driven core-collapse supernova mechanisms.

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Title: Gaia16apd -- a link between fast-and slowly-declining type I superluminous supernovae
Author: T. Kangas, N. Blagorodnova, S. Mattila, P. Lundqvist, M. Fraser, L. K. Hardy, M. D. Stritzinger, E. Cappellaro, N. Elias-Rosa, J. Harmanen, E. Y. Hsiao, E. Kankare, M. B. Nielsen, T. M. Reynolds, L. Rhodes, A. Somero, L. Wyrzykowski

We present ultraviolet, optical and infrared photometry and optical spectroscopy of the type Ic superluminous supernova (SLSN) Gaia16apd, covering its evolution from 27 d before the g-band peak to the nebular phase, including the latest spectrum ever obtained for a fast-declining type Ic SLSN at 150.9 d. Gaia16apd is one of the closest SLSNe known (z=0.102±0.001), with detailed optical and Swift ultraviolet (UV) band observations covering the peak. Gaia16apd is a spectroscopically typical type Ic SLSN, exhibiting the characteristic blue early spectra with Oii absorption, and reaches a peak Mg=-21.8±0.1 mag. However, photometrically it exhibits an evolution intermediate between the fast- and slowly-declining type Ic SLSNe, with an early evolution closer to the fast-declining events. It is unusually UV-bright even for a SLSN, reaching a non-K-corrected M_uvm2 \simeq -23.2 mag, the only other type Ic SLSN with similar UV brightness being SN 2010gx. This event highlights the importance of good rest-frame UV coverage for understanding SLSNe. Assuming that the event was powered by magnetar spin-down, we derive a period of P = 1.9^{+0.3}_{-0.2} ms and a magnetic field of B = 2.1^{+0.5}_{-0.2} x 10^14 G for the magnetar. The estimated ejecta mass is between 6 and 13 solar masses and the kinetic energy between 1.0 and 2.1 x 10^52 erg, depending on opacity. The 150.9 d spectrum shows a remarkable similarity to slowly-declining type Ic SLSNe at late times and implies that the two classes originate from similar progenitors.

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