The Magnetar Model and the Ejecta–Circumstellar-Matter Interaction Model for 31 Luminous, Rapidly Evolving Optical Transients. (arXiv:1904.09604v2 [astro-ph.HE] UPDATED)
<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:+Gan_W/0/1/0/all/0/1">Wen-Pei Gan</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:+Filippenko_A/0/1/0/all/0/1">Alexei V. Filippenko</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:+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>
We study 31 luminous, rapidly evolving optical transients (REOTs), and use
the magnetar model and the ejecta–circumstellar-matter (CSM) interaction (CSI)
model to fit their multiband light curves. We find that 28 events can be fitted
by the magnetar model. and the derived masses ($sim0.05$–5.58,M$_odot$) are
consistent with that of stripped and ultrastripped core-collapse supernovae
(CCSNe). On the other hand, the CSI model can fit 25 events; the derived ejecta
masses are $sim 3$–30,M$_odot$, consistent with that of SNe~Ibn. The
results, together with the fact that many luminous REOTs have been confirmed to
be luminous SNe~IIb/Ib/c or Ibn/IIn, suggest that at least a fraction of
luminous REOTs spectroscopically unclassified might be rapidly evolving
SNe~Ib/Ic or Ibn. Three events in the sample cannot be explained by the two
models we use. We expect that future intense photometry, spectroscopic
classifications, and systematic light-curve modeling of luminous REOTs will
shed more light on their nature.
We study 31 luminous, rapidly evolving optical transients (REOTs), and use
the magnetar model and the ejecta–circumstellar-matter (CSM) interaction (CSI)
model to fit their multiband light curves. We find that 28 events can be fitted
by the magnetar model. and the derived masses ($sim0.05$–5.58,M$_odot$) are
consistent with that of stripped and ultrastripped core-collapse supernovae
(CCSNe). On the other hand, the CSI model can fit 25 events; the derived ejecta
masses are $sim 3$–30,M$_odot$, consistent with that of SNe~Ibn. The
results, together with the fact that many luminous REOTs have been confirmed to
be luminous SNe~IIb/Ib/c or Ibn/IIn, suggest that at least a fraction of
luminous REOTs spectroscopically unclassified might be rapidly evolving
SNe~Ib/Ic or Ibn. Three events in the sample cannot be explained by the two
models we use. We expect that future intense photometry, spectroscopic
classifications, and systematic light-curve modeling of luminous REOTs will
shed more light on their nature.
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