We present a fireball detected in the night sky over Kyoto , Japan on UT 2017 April 28 at { 15 ^ { h } 58 ^ { m } 19 ^ { s } } by the SonotaCo Network .
The absolute visual magnitude is M _ { v } = - 4.10 \pm 0.42 mag .
Luminous light curves obtain a meteoroid mass m =29 \pm 1 g , corresponding to the size a _ { s } =2.7 \pm 0.1 cm .
Orbital similarity assessed by D-criterions ( cf . D _ { 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 \citep [ ] [ ] Pravec07Icar .
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 1 mm 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 .