Modeling the Light Curves of the Luminous Type Ic Supernova 2007D. (arXiv:1904.06598v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wang_S/0/1/0/all/0/1">Shan-Qin Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cano_Z/0/1/0/all/0/1">Zach Cano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_L/0/1/0/all/0/1">Long Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_L/0/1/0/all/0/1">Liang-Duan Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_L/0/1/0/all/0/1">Ling-Jun Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zheng_W/0/1/0/all/0/1">WeiKang Zheng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dai_Z/0/1/0/all/0/1">Zi-Gao Dai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liang_E/0/1/0/all/0/1">En-Wei Liang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Filippenko_A/0/1/0/all/0/1">Alexei V. Filippenko</a>
SN~2007D is a nearby (redshift $z = 0.023146$), luminous Type Ic supernova
(SN) having a narrow light curve (LC) and high peak luminosity. Previous
research based on the assumption that it was powered by the $^{56}$Ni cascade
decay suggested that the inferred $^{56}$Ni mass and the ejecta mass are $sim
1.5$M$_{odot}$ and $sim 3.5$M$_{odot}$, respectively. In this paper, we
employ some multiband LC models to model the $R$-band LC and the color ($V-R$)
evolution of SN~2007D to investigate the possible energy sources powering them.
We find that the pure $^{56}$Ni model is disfavored; the multiband LCs of
SN~2007D can be reproduced by a magnetar whose initial rotational period
$P_{0}$ and magnetic field strength $B_p$ are $7.28_{-0.21}^{+0.21}$ (or
$9.00_{-0.42}^{+0.32}$) ms and $3.10_{-0.35}^{+0.36}times 10^{14}$ (or
$2.81_{-0.44}^{+0.43}times 10^{14}$) G, respectively. By comparing the
spectrum of SN~2007D with that of some superluminous SNe (SLSNe), we find that
it might be a luminous SN like several luminous “gap-filler” optical
transients that bridge ordinary and SLSNe, rather than a genuine SLSN.
SN~2007D is a nearby (redshift $z = 0.023146$), luminous Type Ic supernova
(SN) having a narrow light curve (LC) and high peak luminosity. Previous
research based on the assumption that it was powered by the $^{56}$Ni cascade
decay suggested that the inferred $^{56}$Ni mass and the ejecta mass are $sim
1.5$M$_{odot}$ and $sim 3.5$M$_{odot}$, respectively. In this paper, we
employ some multiband LC models to model the $R$-band LC and the color ($V-R$)
evolution of SN~2007D to investigate the possible energy sources powering them.
We find that the pure $^{56}$Ni model is disfavored; the multiband LCs of
SN~2007D can be reproduced by a magnetar whose initial rotational period
$P_{0}$ and magnetic field strength $B_p$ are $7.28_{-0.21}^{+0.21}$ (or
$9.00_{-0.42}^{+0.32}$) ms and $3.10_{-0.35}^{+0.36}times 10^{14}$ (or
$2.81_{-0.44}^{+0.43}times 10^{14}$) G, respectively. By comparing the
spectrum of SN~2007D with that of some superluminous SNe (SLSNe), we find that
it might be a luminous SN like several luminous “gap-filler” optical
transients that bridge ordinary and SLSNe, rather than a genuine SLSN.
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