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most consistent with RNe and LBVs. Let us now consider  the astrophysical implications of these two possible classifications.  \subsection{Physical Implications of the RN Model}  The physical limits of the RN model are best evaluated by combining  the two key observables of recurrence period and peak brightness. In  this examination we rely on a pair of papers that evaluated an 
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\citet{Yaron:2005} suggest that such systems should have a very low  peak amplitude (barely consistent with the lower limit for \spock) and  a low peak luminosity ($\sim$100 times less luminous than the \spock  events). Thus, if The closest analog for the \spock events from the population of known  RN systems is the nova M31N\,2008a-12. \citet{Kato:2015} provided a  theoretical model that can account for the key observational  characteristics of this remarkable nova: the very rapid recurrence  timescale ($<$1 yr), fast optical light curve ($\t2\sim2$ days), and  short supersoft x-ray phase \citep[6-18 days after optical  outburst][]{Henze:2015a}. To match these observations,  \citeauthor{Kato:2015} invoke a 1.38 \Msun white dwarf primary,  drawing mass from a companion at a rate of $1.6\times10^{-7}$ \Msun  yr$^{-1}$. This is largely consistent with the theoretical  expectations derived by \citet{Yaron:2005}, and reinforces the  conclusion that a combination of a high mass white dwarf and efficient  mass transfer are the key ingredients for rapid recurrence and short  light curves. The one feature that can not be effectively explained  with this scenario is the peculiarly high luminosity of the \spock  events -- even after accounting for the very large uncertainties. If  the \spock transients are in fact two outbursts  from caused by  a single RN system, then that progenitor system would be the most extreme WD binary yet known. \subsection{Physical Implications of the LBV Model}  For the LBV scenario, the observed \spock events would also stand out  as quite extreme. The observed rise and decline times for \spock 
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of energy. This approach assumes that the energy released in an LBV  eruption is generated slowly in the stellar interior and is in some  way ``bottled up'' by the stellar envelope over months or years,  before being released in a rapid mass ejection. The ``build-up'' timescale to match the radiative energy release is then \begin{equation}  \label{eqn:trad} 
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reasonable quiescent luminosity value for the massive ($M>10\Msun$)  progenitor stars expected for LBVs.  Although the above discussion shows that the observations of the  \spock transients are largely consistent with the observed  characteristics of known LBV systems, this does not mean that we have  a viable physical model to explain these events. Rapid transient  episodes in LBVs such as SN 2002kg and SN 2009ip may best be explained  by a sudden ejection of an optically thick shell  \citep[e.g.]{Smith:2010,Smith:2011b}, or by some form of S Dor-type  variability \citep{Weis:2005,VanDyk:2006,Foley:2011}, which may be  driven by stellar pulsation rather than mass ejection  \citep{VanGenderen:1997,VanGenderen:2001}.  For massive stars such as \etacar at its great eruption and the  rapidly varying SN 2009ip, the effective photospheric radius during  eruption must have been comparable to the orbit of Saturn  \citep[$10^{14}$ cm][]{Davidson:1997,Smith:2011,Foley:2011}. With  observed photospheric velocities of order 500 km s$^{-1}$ for such  events, the dynamical timescale is on the order of tens to hundreds of  days. The very rapid light curves of both \spock events will add to  the already challenging task of developing a coherent theoretical  explanation for the physical mechanisms that drive the great eruptions  and the S Dor-type variation of LBVs.  %To examine the temperature and total energy output, we first make a  %set of (admittedly unfounded) assumptions: (1) the two outbursts had a  %very similar SED; (2) the last observed epoch for each event