  We present a fireball detected in the night sky over Kyoto, Japan on UT 2017
April 28 at ${\rm 15^{h}\,58^{m}\,19^{s}}$ by the SonotaCo Network. The
absolute visual magnitude is $M_{\rm v}$=$-$4.10$\pm$0.42mag. Luminous light
curves obtain a meteoroid mass $m$=29$\pm$1g, corresponding to the size $a_{\rm
s}$=2.7$\pm$0.1cm. Orbital similarity assessed by D-criterions (cf. $D_{\rm
SH}$=0.0079) has identified a likely parent, the binary near-Earth asteroid
(164121) 2003 YT$_1$. The suggested binary formation process is a YORP-driven
rotational disintegration (Pravec & Harris 2007). The asynchronous state
indicates the age of $<$10$^4$yr, near or shorter than the upper limit to
meteoroid stream lifetime. We examine potential dust production mechanisms for
the asteroid, including rotational instability, resurfacing, impact,
photoionization, radiation pressure sweeping, thermal fracture and sublimation
of ice. We find some of them capable of producing the meteoroid-scale
particles. Rotational instability is presumed to cause mass shedding, in
consideration of the recent precedents (e.g. asteroid (6478) Gault), possibly
releasing mm-cm scale dust particles. Impacts by micrometeorites with size
$\simeq$1mm could be a trigger for ejecting the cm-sized particles. Radiation
pressure can sweep out the mm-sized dust particles, while not sufficient for
the cm-sized. For the other mechanisms, unprovable or unidentified. The
feasibility in the parental aspect of 2003 YT$_1$ is somewhat reconciled with
the fireball observation, yielding an insight into how we approach potentially
hazardous objects.
