The Unique Type Ib Supernova 2005bf at Nebular Phases: A Possible Birth Event of a Strongly Magnetized Neutron Star

By K. Maeda, Masaomi Tanaka, K. Nomoto, Nozomu Tominaga, K. Kawabata, P. Mazzali, H. Umeda, T. Suzuki, T. Hattori. 2007

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Late-phase nebular spectra and photometry of Type Ib Supernova (SN) 2005bf taken by the Subaru telescope at ~270 and ~310 days since the explosion are presented. Emission lines ([O I] λλ6300, 6363; [Ca II] λλ7291, 7324; and [Fe II] λ7155) show a blueshift of ~1500-2000 km s-1. The [O I] doublet shows a doubly peaked profile. The line luminosities can be interpreted as coming from a blob or jet containing only ~0.1-0.4 M☉, in which ~0.02-0.06 M☉ is 56Ni synthesized at the explosion. To explain the blueshift, the blob should either be unipolar, moving at the center-of-mass velocity v ~ 2000-5000 km s-1, or suffer from self-absorption within the ejecta, as seen in SN 1990I. In both interpretations, the low-mass blob component dominates the optical output both at the first peak (~20 days) and at the late phase (~300 days). The low luminosity at the late phase (the absolute R magnitude MR ~ -10.2 mag at ~270 days) sets the upper limit for the mass of 56Ni ≲ 0.08 M☉, which is in contradiction to the value necessary to explain the second, main peak luminosity (MR ~ -18.3 mag at ~40 days). Encountered by this difficulty in the 56Ni heating model, we suggest an alternative scenario in which the heating source is a newly born, strongly magnetized neutron star (a magnetar) with the surface magnetic field Bmag ~ 1014-1015 G and the initial spin period P0 ~ 10 ms. Then, SN 2005bf could be a link between normal SNe Ib/c and an X-ray flash associated SN 2006aj, connected in terms of Bmag and/or P0.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

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Citations in the corpus

High luminosity, slow ejecta and persistent carbon lines: SN 2009dc challenges thermonuclear explosion scenarios (2010, background): “Compared to CSM interaction as an alternative non-radioactivity-related energy source, heating from a compact remnant has the advantage that the energy is injected at the centre and released on photon diffusion time-scales, which allows the light curve to rise smoothly to peak (Maeda et al. 2007).”
Observational and Physical Classification of Supernovae (2016, unknown): “Tominaga et al. (2005), Maeda et al. (2007) and Maund et al. (2007) present additional observations and analysis of this unique event.”
A burst in a wind bubble and the impact on baryonic ejecta: high-energy gamma-ray flashes and afterglows from fast radio bursts and pulsar-driven supernova remnants (2016, background): “…(e.g., Vietri & Stella 1998; Inoue, Guetta & Pacini 2003), energetic SNe such as super-luminous SNe (SLSNe) (e.g., Thompson, Chang & Quataert 2004; Maeda et al. 2007; Kasen & Bildsten 2010; Woosley 2010; Murase et al. 2015; Kashiyama et al. 2016), and kilonovae/macronovae (e.g., Kisaka, Ioka…”
Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, background): “However, Maeda et al. (2007), from nebular spectral modelling, find that 0.08 M of 56Ni was synthesized, inconsistent with an 56Ni-powered explanation for the second peak.”
BRIGHT SUPERNOVAE FROM MAGNETAR BIRTH (2009, background): “Indeed, Maeda et al. (2007) have suggested a pulsar as the possible source powering the second (principal) maximum of the light curve of SN 2005bf.”
OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, background): “SN 2005bf had peculiar late-time spectra (Maeda et al. 2007; Modjaz et al. 2008b) and a pronounced and unique double-peaked light curve (Tominaga et al. 2005; Folatelli et al. 2006).”
ANALYTICAL LIGHT CURVE MODELS OF SUPERLUMINOUS SUPERNOVAE: χ2-MINIMIZATION OF PARAMETER FITS (2013, background): “…to explain the LCs of some SLSNe such as SN 2008es and SN 2007bi is that of the energy released by the spin-down of a young magnetar located in the center of the SN ejecta (hereafter the “MAG” model; Ostriker & Gunn 1971; Arnett & Fu 1989; Maeda et al. 2007; Kasen & Bildsten 2010; Woosley 2010).”
THE r-PROCESS NUCLEOSYNTHESIS IN THE VARIOUS JET-LIKE EXPLOSIONS OF MAGNETOROTATIONAL CORE-COLLAPSE SUPERNOVAE (2015, background): “Our results have the amount of Ni-isotopes in the range of M(56Ni) ≤ 0.08M⊙ with ∼ 1014 – 1015 G, which are values for magnetar formation scenario (Maeda et al. 2007b).”
COMPACT REMNANT MASS FUNCTION: DEPENDENCE ON THE EXPLOSION MECHANISM AND METALLICITY (2011, background): “As we discussed, magnetar-strength magnetic fields can also drive outflows, preventing fallback (e.g., Maeda et al. 2007; Kasen & Bildsten 2010).”
FROM SHOCK BREAKOUT TO PEAK AND BEYOND: EXTENSIVE PANCHROMATIC OBSERVATIONS OF THE TYPE Ib SUPERNOVA 2008D ASSOCIATED WITH SWIFT X-RAY TRANSIENT 080109 (2008, background): “If the blueshift continues to remain constant over time (as seen in SN 1996N; Sollerman et al. 1998), then bulk blueshifts or unipolar blob ejections might need to be invoked as suggested for SN 2005bf (Maeda et al. 2007).”
On the nature of supernovae Ib and Ic (2012, background): “This unique transition has been seen for SN2005bf by Folatelli et al. (2006), although mixing is unlikely the cause in this special case (Maeda et al. 2007).”
SUPERNOVA LIGHT CURVES POWERED BY YOUNG MAGNETARS (2009, background): “Maeda et al. (2007) previously raised this possibility for the Type Ib SN 2005bf, and Woosley (2009) has independently shown their relevance as well.”
Superluminous supernovae: 56Ni power versus magnetar radiation (2012, background): “An alternative means to produce a bright display is by magnetar radiation (Wheeler et al. 2000; Maeda et al. 2007; Kasen & Bildsten 2010; Woosley 2010).”
Core-collapse explosions of Wolf–Rayet stars and the connection to Type IIb/Ib/Ic supernovae (2011, background): “The “anomaly” with SN 2005bf is the bright second peak, which does not seem to stem from decay energy but seems more consistent with the birth of a magnetar (Maeda et al. 2007). c© 2010 RAS, MNRAS000, 1–23 but already by 5 d the SN re-brightens.”
GENERALIZED SEMI-ANALYTICAL MODELS OF SUPERNOVA LIGHT CURVES (2011, methodology): “Recently, Kasen & Bildsten (2010) and Woosley (2010) considered models of SLSN LCs powered by the spin-down of a young magnetar (see also Ostriker & Gunn 1971; Arnett & Fu 1979; Maeda et al. 2007).”
Light-curve modelling of superluminous supernova 2006gy: collision between supernova ejecta and a dense circumstellar medium (2012, background): “If the radiation energy released at the magnetar can be converted to thermal energy, the SN ejecta surrounding the magnetar is heated up and the SN can become very bright (Kasen & Bildsten 2010; Woosley 2010; see also Maeda et al. 2007).”