Comet 1P/Halley is the source of
the Orionid and
η
Aquariid meteor showers [1]. The
latter one takes place during
the second encounter of
the Earth with 1P/Halley debris in October, when our
planet is as close as 0.16 AU from the comet's orbit
[2]. A striking feature of 1P meteoroid streams is their
filamentary structure, which has been explained on the
basis of an orbital evolution affected by major planets,
particularly Jupiter [3]. Besides, several authors have
noted that the activity of the Orionid meteor shower
varies significantly from year
to year [4, 5]. In fact, it
has been a source of important meteor outbursts [6].
The last of these took place in 2006 [7]. In order to
increase our knowledge about this stream, the SPanish
Meteor Network (SPMN) ha
s performed in the recent
years a continuous monitoring of the Orionid shower
during its activity period by means of high-sensitivity
CCD video devices. Thus, for instance, although no
remarkable activity was observed during 2010, we
could image several fireballs from this shower. In this
work we analyze one of these events, which was re-
corded together with its emission spectrum on Oct. 23,
2010 at 23h53m09.3
±
0.1s UTC and was named SPMN
231010