A Two-Component Model for the Light Curves of Hypernovae

By K. Maeda, P. Mazzali, J. Deng, K. Nomoto, Y. Yoshii, H. Tomita, Yukiyasu Kobayashi. 2003

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The light curves of hypernovae, i.e., very energetic supernovae with E51 ≡ E/1051 ergs ≳5-10, are characterized by a phase of linear decline at epochs of a few months. Classical, one-dimensional explosion models fail to simultaneously reproduce the light curve near peak and at the linear decline phase. The evolution of these light curves may, however, be explained by a simple model consisting of two concentric components. The outer component is responsible for the early part of the light curve and for the broad absorption features observed in the early spectra of hypernovae, similar to the one-dimensional models. In addition, a very dense inner component is added, which reproduces the linear decline phase in the observed magnitude versus time relation for SN 1998bw, SN 1997ef, and SN 2002ap. This simple approach does contain one of the main features of jet-driven, asymmetric explosion models, namely, the presence of a dense core. Although the total masses and energies derived with the two-component model are similar to those obtained in previous studies that also adopted spherical symmetry, this study suggests that the ejecta are aspherical, and thus, the real energies and masses may deviate from those derived assuming spherical symmetry. The supernovae that were modeled are divided into two groups according to the prominence of the inner component: the inner component of SN 1997ef is denser and more 56Ni-rich, relative to the outer component, than the corresponding inner components of SN 1998bw and SN 2002ap. These latter objects have a similar inner-to-outer component ratio, although they have very different global values of mass and energy.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/baac525cf806f1184460c71ccc68a9bed180a65b

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Citations in the corpus

The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, methodology): “An example of this is the grey-dashed line in Figure 9, which is an analytical model [122, 213] that considers the luminosity produced by a fiducial SN with a kinetic energy of EK = 25 × 10 51 erg, an ejecta mass ofMej = 6M⊙, and a nickel mass ofMNi = 0.”
The Unique Type Ib Supernova 2005bf at Nebular Phases: A Possible Birth Event of a Strongly Magnetized Neutron Star (2007, methodology): “Taking Mej,neb, Eneb,51, and M(56Ni)neb from Table 1, we use equations (1 – 3) of Maeda et al. (2003) with the modification to include contribution from the 56Ni → 56Co decay.”
The Type Ic Hypernova SN 2003dh/GRB 030329 (2003, methodology): “Here we can follow the same approach as in the two-component models of Maeda et al. (2003), as this is essentially the same problem.”
The Broad-lined Type Ic SN 2003jd (2007, background): “This was already noted by Maeda et al. (2003), who obtained a fair overall fit to the light curves of SNe Ic by schematically dividing the SN ejecta into two regions: a highdensity inner region and a low-density outer region with high and low γ-ray trapping, respectively.”
Fourteen months of observations of the possible super-Chandrasekhar mass Type Ia Supernova 2009dc (2010, methodology): “…nickel mass produced by SN 2009dc from latetime photometry, we write out the SN luminosity as a function of time (e.g. Clocchiatti & Wheeler 1997; Maeda et al. 2003, 2009), L(t) = MNi ( εγ (1 − e−τ (t)) + fe+εe+ ) e−t/111.3 (2) where t is the number of days from the explosion date, MNi is the…”
Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, methodology): “…extent, SNe IcBL) means the EK and Mej estimates here may be underestimates as we make no account of the contribution from a denser, inner core of material that will reveal itself only in the late-time light curves, and which may have a significant contribution in SNe Ic-BL (Maeda et al. 2003).”
The Rates of Hypernovae and Gamma-Ray Bursts: Implications for Their Progenitors (2004, background): “…that appear less powerful may simply be viewed off-axis, leading to an underestimation of the kinetic energy and to the non-detection of the GRB. SN 2002ap could be such a case, since there is ample evidence that the explosion was aspherical, like SN 1998bw (Mazzali et al. 2002, Maeda et al. 2003).”
Nebular emission-line profiles of Type Ib/c supernovae - Probing the ejecta asphericity (2009, background): “Note that the presence of dense cores has been suggested for several SNe to explain their line profiles and late-time light-curve slopes (Iwamoto et al. 2000; Mazzali et al. 2000; Maeda et al. 2003; Mazzali et al. 2007a,b).”
The Supernova Gamma-Ray Burst Connection (2006, background): “These observations are best explained in a two component model (Maeda et al., 2003; Woosley and Heger, 2003) in which the the supernova has a high velocity along its rotational axes, reflecting the activity of some jet-like energy source, and low velocities in the equator.”