IMO INFO(2-18)

1International Meteor Organization

2019 Meteor Shower Calendar
edited by Jürgen Rendtel 1

1

Introduction

Welcome to the twenty-ninth edition of the International Meteor Organization (IMO) Meteor
Shower Calendar. We intend to draw the attention of observers to both regularly returning
meteor showers and to events which may be possible according to model calculations. We may
experience additional peaks and/or enhanced rates but also the observational evidence of no rateor density enhancement. The position of peaks and data of shower meteor magnitudes along
the stream are important information. Such data may help to improve our knowledge about theeffects and interactions from the release of a meteoroid from its parent object until it enters ouratmosphere. Further, the Calendar hopefully continues to be a useful tool to plan your meteor
observing activities.
Nowadays, video meteor networks are operational throughout the year which are less affectedby moonlit skies than visual observers. So we refer to the moonlight conditions first of all forthe visual observer. The moonlight circumstances for observations of the three strongest annual
shower peaks bring essentially new Moon for the Quadrantids, a waxing gibbous Moon for the
Perseids and full Moon for the Geminids. Conditions for the maxima of the Lyrids (shortly
after full Moon), the Orionids and the Leonids (last quarter) will strongly interfere with visualobservations. The η-Aquariids are well observable (new Moon), while the Southern δ-Aquariids
and the Ursids reach their maxima close to the new Moon. The Draconids see a waxing gibbous
Moon.
Some interesting events are announced for 2019, although no spectacular outburst is predicted.
Since there is always a possibility of completely unexpected events, ideally meteor observing
should be performed throughout the year. While often there are many observers active during
periods of high or medium activity, one should keep in mind that new events may happen
at other times too. Continuous monitoring is possible with automated video systems and byradio/radar systems, but is also worthwhile for visual observers during moon-free nights. Thisway we can improve the data for established sources, including their outer ranges. Combining
data obtained with different techniques may increase the reliability of derived quantities and is
helpful for calibrating purposes. Since regular visual observations may be impractical for many
people, however, one of the aims of the Shower Calendar is to highlight times when a particulareffort might be most usefully employed. It indicates as well specific projects which need goodcoverage and attention.
1

Based on information in the Meteor Observers Workbook 2014, edited by Jürgen Rendtel (referred to as ‘WB’
in the Calendar), and “A Comprehensive List of Meteor Showers Obtained from 10 Years of Observations with
the IMO Video Meteor Network” by Sirko Molau and Jürgen Rendtel (referred to as ‘VID’ in the Calendar),as amended by subsequent discussions and additional material extracted from data analyses produced since.
Particular thanks are due to David Asher, Peter Jenniskens, Hutch Kinsman, Esko Lyytinen, Mikhail Maslov,
Mikiya Sato and Jérémie Vaubaillon for new information and comments in respect of events in 2019 (see also theReferences in section 9). Koen Miskotte provided the information for the SDA and CAP activity in late July.

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The heart of the Calendar is the Working List of Visual Meteor Showers (Table 5 on page 24)
which is continuously updated so that it is the most accurate listing available today for visualmeteor observing. Nevertheless, it is a Working List which is subject to further modifications,based on the best data we had at the time the Calendar was written. Observers should always
check for later changes noted in the IMO’s journal WGN or on the IMO website. Vice versa, weare always interested to receive information whenever you find any anomalies! To allow for better
correlation with other meteor shower data sources, we give the complete shower designation
including the codes taken from IAU’s Meteor Data Center listings.
Video meteor observations allow us to detect weak sources. An increasing number of confirmed
radiants provides us with more possibilities to establish relations between meteoroid streams
and their parent objects. Some of the sources may produce only single events but no annual
recurring showers, such as, for example, the June Bootids and the October Draconids. From
stream modelling calculations we know that one meteoroid stream may cause several meteor
showers, and that a stream may be related to more than one parent object.
Observing techniques which allow the collection of useful shower data include visual, video andstill-imaging along with radar and radio forward scatter methods. Visual and video data allow
rate and flux density calculations as well as determination of the particle size distribution interms of the population index r or the mass index s. Multi-station camera setups provide us
with orbital data, essential for meteoroid-stream investigations. Showers with radiants too near
the Sun for observing by the various optical methods can be detected by forward-scatter radioor back-scatter radar observations – although attempts with optical observations can be useful
too. Some of the showers are listed in Table 7, the Working List of Daytime Meteor Showers.
The IMO’s aims are to encourage, collect, analyze, and publish combined meteor data obtained
from sites all over the globe, to improve our understanding of the meteor activity detectablefrom the Earth’s surface. For best effects, it is recommended that all observers should follow
the standard IMO observing guidelines when compiling information, and submit those data
promptly to the appropriate Commission for analysis (contact details are at the end of the
Calendar). Many analyses try to combine data obtained by more than one method, extending
the ranges and coverage but also to calibrate results from different techniques. Thanks to theefforts of the many IMO observers worldwide since 1988 that have done this, we have been able
to achieve as much as we have to date, including keeping the shower listings vibrant. This is nota matter for complacency however, since it is solely by the continued support of many people
across the planet that our attempts to construct a better and more complete picture of thenear-Earth meteoroid flux can proceed.
Timing predictions are included below and on all the more active night-time and daytime shower
maxima as reliably as possible. However, it is essential to understand that in many cases, suchmaxima are not known more precisely than to the nearest degree of solar longitude. In addition,
variations in individual showers from year to year mean past returns are only a guide as to wheneven major shower peaks can be expected. As noted already, the information given here may be
updated and added-to after the Calendar has been published. Some showers are known to show
particle mass-sorting within their meteoroid streams, so the radar, radio, still-imaging, video
and visual meteor maxima may occur at different times from one another, and not necessarily
just in those showers. The majority of data available are for visual shower maxima, so this must
be borne in mind when employing other observing techniques.
However and whenever you are able to observe, we wish you all a most successful year’s workand very much look forward to receiving your data, whose input is possible via the online formon the IMO’s website www.imo.net. Clear skies!

IMO INFO(2-18)

23Antihelion Source

The Antihelion Source (ANT) is a large, roughly oval area of about 30◦ in right ascension and
15◦ in declination, centred about 12◦ east of the solar opposition point on the ecliptic, hence
its name. It is not a true shower at all (hence it has no IAU shower number), but is rather aregion of sky in which a number of variably, if weakly, active minor showers have their radiants.
Until 2006, attempts were made to define specific showers within this complex, but this often
proved very difficult for visual observers to achieve. IMO video results have shown why, becauseeven instrumentally, it was impossible to define distinct and constantly observable radiants formany of the showers here! Thus we recommend observers simply to identify meteors from thesestreams as coming from the ANT alone. Apart from this, we have been able to retain the JulyAugust α-Capricornids, and particularly the Southern δ-Aquariids as apparently distinguishable
showers separate from the ANT. Later in the year, the Taurid showers dominate the activity
from the Antihelion region meaning the ANT should be considered inactive while the Taurids areunderway, from early September to early December. To assist observers, a set of charts showing
the location for the ANT and any other nearby shower radiants is included here, to complement
the numerical positions of Table 6 (page 25), while comments on the ANT’s location and likely
activity are given in the quarterly summary notes.

3

January to MarchThe year starts with two events on January 4: the Quadrantid (010 QUA) peak for thenorthern hemisphere observers probably close to 2h UT. According to model calculations by
Mikhail Maslov, the trail of meteoroids ejected from comet 46P/Wirtanen in 1974 passes
the Earth at 0.00048 au distance on January 4, 18h26m UT. There is some similarity of theejection of Draconid meteoroids which produced activity in 1999. The estimated ZHR may be
about 10, dominated by faint optical and radio meteors. The radiant is located at α = 337◦,
δ = −3◦ , between the stars γ and κ Aquarii. At the calculated time, the Sun is below thehorizon in Europe and most parts Africa. The radiant elevation is ≈ 45◦ in the western Sahara,≈ 35◦ on the Iberian peninsula and lower further east.
Conditions regarding moon-free observations become worse towards the maximum of the γ Ursae Minorids (404 GUM) around January 12–15. Some late parts of the long-lasting December Leonis Minorids (032 DLM) can be traced until early February. The southernhemisphere’s α-Centaurids (102 ACE) can be well observed in early February and the possible minor γ-Normids (118 GNO) of March are partly affected by moonlight (first quarter
Moon on March 14).
In Table 3 of Peter Jenniskens’ (2006) book possible activity from the 1-revolution dust trailof comet C/1907 G1 (Grigg-Mellish) is listed for March 31, 17h 26m UT from a radiant at
α = 309◦ , δ = −60◦ (which is south of α Pavonis). There is no moonlight interference this time.
A possible encounter of the same trail on 2018 March 31 was noted in the same source as “far”
and no activity has been reported (this happened close to full Moon). It is worth to check for
activity and timing as it may help us to improve our understanding of stream evolution.
The ANT’s radiant centre is situated in south-east Gemini in January, and crosses Cancer
during much of the month, before passing into southern Leo for most of February. It then glides
through southern Virgo during March. ANT ZHRs should be expected at a level of 2 − 3 formost of the time. IMO analyses of visual and video data have suggested some ill-defined minor
maxima with ZHRs ≈ 3 at various positions. A slight increase derived from video flux data may
occur around λ⊙ ≈ 355◦ (2019 March 17).

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30
Jan 102030
Feb 1020
Mar 1020

ANT (Jan–Mar)
A short outburst of the κ-Cancrids (793 KCA) was found on 2015 January 10 at 02h 50m UT(λ⊙ = 289 ◦. 315) in radar and video data. The radiant was at α = 138◦, δ = +9◦ ). Activity was
also detected in the 2016 video data (Molau et al., 2016a). Although there are no visual data
available yet, observers are encouraged to check especially the period around 2019 January 10,
03h − 04h UT for possible activity. The radiant of the Antihelion source centre is at α = 122◦ ,δ = +19◦ , i.e. roughly 20◦ southeast, and the KCA meteors (V∞ = 47 km/s) are faster than the
ANT (V∞ = 30 km/s).
Expected approximate timings for the daytime shower maxima this quarter are:Capricornids/Sagittariids (115 DCS) – February 1, 24h UT and χ-Capricornids (114 DXC) –February 13, 23h UT. Recent radio results have implied the DCS maximum may fall variably
sometime between February 1–4 however, while activity near the expected DXC peak has tended
to be slight and up to a day late. Both showers have radiants < 10◦ –15◦ west of the Sun at
maximum, so cannot be regarded as visual targets even from the southern hemisphere.
Quadrantids (010 QUA)
Active: December 28–January 12; Maximum: January 4, 02h 20m UT (λ⊙ = 283 ◦. 16),
ZHR = 120 (can vary ≈ 60–200);
Radiant: α = 230◦, δ = +49◦ ; Radiant drift: see Table 6;
V∞ = 41 km/s; r = 2.1 at maximum, but variable.
New Moon on January 6 creates optimum viewing conditions for the expected Quadrantid maximum on January 4. For many northern hemisphere sites, the shower’s radiant is circumpolar,
in northern Boötes, from where it first attains a useful elevation after local midnight, steadily
improving through till dawn. The 02h UT timing for the peak will be favourable for European
longitudes. The λ⊙ = 283 ◦. 16 maximum timing is based on the best-observed return of theshower ever analysed, from IMO data collected in 1992, as confirmed by radio results in mostyears since 1996. It also coincides with the closest approach to the stream calculated by Jérémie
Vaubaillon (λ⊙ = 283 ◦. 17). The peak is short-lived with an average duration (full width at halfmaximum) of about four hours. Hence it can be easily missed if the observer is located outside
the “main observing window” (high radiant in nighttime) or just a few hours of poor northernwinter weather. An added level of complexity comes from the fact mass-sorting of particles
across the meteoroid stream related to the comet 96P/Machholz and the minor planet 2003 EH1

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5

may make fainter objects (radio and telescopic meteors) reach maximum up to 14 hours before
the brighter (visual and photographic) ones. Mass segregation effects have also been found for asmall peak preceding the main maximum in 2016. On a few returns, a maximum following themain visual one by some 9–12 hours occurred in radio data. Visual confirmation of any repeat ofsuch behaviour would be welcomed. Therefore observers should be alert throughout the shower
activity period. QUA activity tends to be very low more than a day or so from the peak, butbright shower meteors may also occur in some nights around the peak on either side. The New
Moon period leaves enough room to collect data of the outer range of the shower which is not
yet well studied.

QUA

Dec 30
Jan 0105
1015

γ-Ursae Minorids (404 GUM)
Active: January 10–22; Maximum: around January 18 (λ⊙ = 298◦); ZHR ≈ 3;
Radiant: α = 228◦ , δ = 67◦ ; Radiant drift: see Table 6;
V∞ = 31 km/s; r = 3.0.
Little is yet known about this minor shower which has been detected in video and visual data
recently and has been annually observed. Considering the velocity, meteors from this far northernradiant should be similar to the Ursids in their appearance. All data about the activity period
and shower parameters should be treated as tentative and need further confirmation. First
quarter Moon on January 14 allows observations mainly before the given maximum.

Jan 10
15
GUM

20
25

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α-Centaurids (102 ACE)
Active: January 31–February 20; Maximum: February 8, 13h UT (λ⊙ = 319 ◦. 2);
ZHR = variable, usually ≈ 6, but may reach 25+;
Radiant: α = 210◦, δ = −59◦ ; Radiant drift: see Table 6;
V∞ = 58 km/s; r = 2.0.

The α-Centaurids are one of the main southern summer high points occasionally including
bright meteors or fireballs. The average peak ZHR between 1988–2007 was merely 6 though(WB, p. 18), albeit coverage has often been very patchy. Despite this, in 1974 and 1980, burstsof only a few hours’ duration apparently yielded ZHRs closer to 20–30. Significant activity wasreported on 2015 February 14 (airborne observation) although there was no confirmation of an
outburst predicted for 2015 February 8. Further data is needed to obtain information about thestructure and extension of the stream. The listed activity period is based on recent video data.
The shower’s radiant is nearly circumpolar for much of the sub-equatorial inhabited Earth, andis at a useful elevation from late evening onwards. This year the maximum period falls a few
days after new Moon and is therefore favourable for dark-sky coverage of the entire night.
γ-Normids (118 GNO)
Active: February 25–March 28; Maximum: March 15 (λ⊙ = 354◦ ); ZHR = 6;
Radiant: α = 239◦, δ = −50◦ , Radiant drift: see Table 6;
V∞ = 56 km/s; r = 2.4.

GNO
20

Mar 1028

Feb 20IMO INFO(2-18)

7For most of their activity, γ-Normid ZHRs seem to be virtually undetectable above the background sporadic rate. An analysis of IMO data from 1988–2007 showed an average peak ZHRof ≈ 6 at λ⊙ = 354◦ , with ZHRs < 3 on all other dates during the shower (HMO, pp. 131–132).
Results since 1999 have suggested the possibility of a short-lived peak alternatively between
λ⊙ ≈ 347◦ –357◦ , equivalent to 2019 March 8–18. A later analysis of video data obtained only
from locations south of the equator has indicated that the activity occurs preferentially around
March 25 (λ⊙ = 4◦ ) instead, from a radiant at α = 246◦, δ = −51◦ . Post-midnight watchingyields better results, when the radiant is rising to a reasonable elevation from southern hemisphere sites (the radiant does not rise for many northern ones). Moonlight circumstances are
best for the March 15 period (just after first quarter) but will strongly interfere with the possible
late maximum timing.

4

April to June

Meteor activity increases towards the April-May boundary, particularly caused by opticallyunobservable (daytime) showers. Full Moon on April 19 completely ruins the Lyrid (006
LYR) maximum on April 23 around 0h UT (at 32 ◦. 32). The waning gibbous Moon leaves a little
time in the evening for the π-Puppid (137 PPU) maximum which should occur near 6h UT
on April 24. In 2019, both the η-Aquariid (031 ETA) maximum period, due around May 5,
and the η-Lyrids (145 ELY) with a potential peak on May 9 or slightly later can be perfectly
observed in moonless nights. The potential peak periods of the June Bootids (170 JBO) see
a waning crescent Moon (last quarter on June 25).

20
Mar 102030
Apr 102030
May 1020

ANT (Mar–May)
According to analyses of visual and video IMO data, the ANT should produce ZHRs between
2 and 4 with insignificant variations. There may be a rather slow increase towards end-May
followed by a decrease into July. The radiant area drifts from south-east Virgo through Librain April, then across the northern part of Scorpius to southern Ophiuchus in May, and on into
Sagittarius for much of June.

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20

Jul 1030

20

Jun 1030

20

May 1030

20

ANT (May–Jul)
Daytime showers: In the second half of May and throughout June, most of the annual meteor
action switches to the daylight sky, with several shower peaks expected during this time. For
radio observers, the expected UT peak times for these showers are as follows:
April Piscids (144 APS) – April 23, 4h ;ε-Arietids (154 DEA) – May 9, 21h ;May Arietids (294 DMA) – May 16, 22h ;o-Cetids (293 DCE) – May 20, 21h ;Arietids (171 ARI) – June 7, 22h (more details see page 10);
ζ-Perseids (172 ZPE) – June 9, 24h ;β-Taurids (173 BTA) – June 28, 23h.
Signs of most were found in radio data from 1994–2008, though some are difficult to define
individually because of their proximity to other radiants. The maxima of the Arietids and ζPerseids tend to blend into one another, producing a strong radio signature for several days inearly to mid June. The shower maxima dates are not well established and may deviate from thegiven times. There seems to be a modest recurring peak around April 24 as well, perhaps due
to combined rates from the first two showers listed here, and possibly the δ-Piscids, which we
previously listed as having a peak on April 24, although the IAU seems not to recognise this asa genuine shower. Similarly, there are problems in identifying the o-Cetids in the IAU stream
lists. The current number and abbreviation given here for it is actually for the IAU source called
the “Daytime ω-Cetid Complex”, because that seems a closer match to the o-Cetids as definedby earlier reports.
η-Aquariids (031 ETA)
Active: April 19–May 28; Maximum: May 6, 14h UT (λ⊙ = 45 ◦. 5);
ZHR = 40 (periodically variable, ≈ 40–85);
Radiant: α = 338◦, δ = −1◦ ; Radiant drift: see Table 6;
V∞ = 66 km/s; r = 2.4.
This stream is associated with Comet 1P/Halley, like the Orionids of October. Shower meteors
are only visible for a few hours before dawn essentially from tropical and southern hemispheresites. Some useful results have come even from places around 40◦ N latitude at times however.
Further north, observers can expect only few occasional shower meteors. The ETA is one of theIMO INFO(2-18)

9best for southern observers and would benefit from increased observer activity generally. The
fast and often bright meteors make the wait for radiant-rise worthwhile, and many events leaveglowing persistent trains. While the radiant is still low, η-Aquariids tend to have very longpaths, which can mean observers underestimate the angular speeds of the meteors, so extra careis needed for meteor shower association.

A relatively broad maximum, sometimes with a variable number of submaxima, occurs aroundMay 5–6. IMO analyses of the general activity profile based on data collected between 1984–
2001, have shown that the ZHR is generally above 30 in the period May 3–10. The peak rates
appear to be variable on a roughly 12-year timescale. Assuming this Jupiter-influenced cycle isreal, the next ”peak” is due around 2020–2022, so ZHRs should be better than in the previous
years. Activity around the most recent ZHR peak period in 2008 and 2009 reached ≈ 85 and 65,
respectively. In 2013, ZHRs up to ≈ 70 have been recorded (WB, p. 24), and the 2017 returnyielded a peak ZHR of 75 as well.
Modelling of the stream by Mikhail Maslov yields two trail encounters for 2019. The times forthese are May 4, between 4 − 10h UT (meteors from −539) and May 6, 12 − 20h UT (−985 trail).
Both may add 5 − 10 to the general rate.
New Moon on May 4 creates ideal viewing conditions this year. All forms of observing can beused to study it, with radio work allowing activity to be followed even from many northernlatitude sites throughout the daylight morning hours. The radiant culminates at about 08h local
time.
η-Lyrids (145 ELY)
Active: May 3–14; Maximum: May 9 (λ⊙ = 48 ◦. 4); ZHR = 3;
Radiant: α = 287◦ , δ = +44◦ ; Radiant drift: see Table 6;
V∞ = 43 km/s; r = 3.0.
This weak shower is associated with Comet C/1983 H1 IRAS-Araki-Alcock. Most of the recent
observational data on it has come from video results, which have suggested the maximum mightfall at λ⊙ = 50◦ instead (if so, on 2019 May 11). There is little evidence from visual observations
as yet, but the discussion on p. 25 of WB has more information. Video as well as careful visualplotting will be needed to separate any potential η-Lyrids from the sporadics. The generalradiant area is usefully on-view all night from the northern hemisphere (primarily), with very
little Moon interference around May 9–11 this year.

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Daytime Arietids (171 ARI)
Active: May 14–June 24 (uncertain); Maximum: June 08 (λ⊙ = 76 ◦. 6); ZHR ≈ 30(?);
Radiant: α = 44◦ , δ = +24◦ ; Radiant drift: see Table 6;
V∞ = 38 km/s; r = 2.8.
The radiant is located only about 30◦ west of the Sun. Despite that, a few optical observations
have been repeatedly reported from it in the past. However, its low radiant elevation by thetime morning twilight is too bright means the number of shower meteors recorded by individual
video or visual observers is always low. Consequently, an ongoing IMO project to pool data on
the shower using all techniques was initiated in 2014, to combine results from many independent
observing intervals, even those periods which contain few, or even no ARI meteors. The currently
available video data do not show a clear profile but a recognizable activity level over a week or so.
Hence all contributions for this project will be most welcome! Since both the correction factor
for radiant elevation and the observing conditions change rapidly in the approach to morning
twilight in early June, it is recommended that visual observers break their watches into shortintervals (of the order of about 15 minutes), determining the limiting magnitude frequently
for each interval. Observers at latitudes south of about 30◦ N are better placed because of thesignificantly poorer twilight conditions further north in June.
June Boötids (170 JBO)
Active: June 22–July 2; Maximum: June 27, 22h UT (λ⊙ = 95 ◦. 7), but see text;
ZHR = variable, 0–100+;
Radiant: α = 224◦, δ = +48◦ ; Radiant drift: see Table 6;
V∞ = 18 km/s; r = 2.2.
This source was reinstated on the Working List only after its unexpected return of 1998 (ZHR
50 − 100+ for more than half a day). Another outburst of similar length (ZHR ≈ 20 − 50) was
observed on 2004 June 23. The return predicted in 2010 yielded a poorly established ZHR < 10
on June 23–24. Prior to 1998, only three more probable returns had been detected, in 1916, 1921
and 1927 (however, with different reliability). Since there were no significant reports between
1928 and 1997, it seemed likely these meteoroids no longer encountered Earth. The parent comet
7P/Pons-Winnecke has an orbit that now lies around 0.24 astronomical units outside the Earth’s
at its closest approach. Its latest perihelion passage occurred on 2015 January 30 (orbital period
about 6.4 years). The 1998 and 2004 events resulted from material ejected from the comet in
the past which now lies on slightly different orbits to the comet itself. For the 2019 return, there
are no predictions of peculiar activity published.

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11

We encourage all observers to routinely monitor throughout the proposed period, in case of
any activity. From mid-northerly latitudes the radiant is observable almost all night, but the
prolonged – in some places continuous – twilight overnight keeps the useable time short. This
year, the Moon reaches its last quarter on June 25. VID suggested some June Boötids may
be visible in most years around June 20 − 25 but with activity largely negligible except nearλ⊙ = 92◦ (2019 June 24), radiating from an area about ten degrees south of the radiant foundin 1998 and 2004, close to α = 216◦ , δ = +38◦.

5

July to September

20
Sep 10
30

ANT

20
SDA
20 15

Aug 1010Aug 0530

CAP
10
Aug 05

30

30
25 20

15Jul 10

25

20
15

20

10
Jul 10

PAU
10

Jul 0530

Aug 0530

25

20
Jul 15The ANT is the chief focus for visual attention during most of July, as its radiant area moves
steadily through eastern Sagittarius, then across northern Capricornus into southwest Aquariuswith ZHRs of ≈ 2 to 3. The large ANT radiant area overlaps that of the minor α-Capricornids(001 CAP) in July–August, but the lower apparent velocity of the CAP allows observers toseparate the two. The Southern δ-Aquariids (005 SDA) are faster and strong enough, and
the Piscis Austrinids (183 PAU) have a radiant distant enough from the ANT area, that12

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both should be more easily separable from the ANT, particularly from the southern hemisphere.
New Moon on August 1 allows us to monitor the activity during the period of highest rates fromthese southern radiants which are due on July 27 (PAU) and July 30 (CAP, SDA), respectively.
On 2016 July 28 at 00h 07m UT a remarkable outburst (ZHR probably of the order of 100) of
the July γ-Draconids (184 GDR) was detected by radar and video observations (Molau etal., 2016b). The same position is reached again on 2019 July 28 near 18h 30m UT. When writing
this text, the return to the respective position on 2018 July 28 has still to come, but whatever
happens in 2018, it is well worth a check whether something is observable around this time. The
radiant is at α = 280◦ , δ = +51◦ , and the meteors have medium speed (V∞ = 27 km/s).
First quarter Moon on August 7 allow the observers to record the ascend towards the maximumof the Perseids (007 PER) which is due between λ⊙ ≈ 139 ◦. 8 to 140 ◦. 3, equivalent to 2019
August 13 02h to 15h UT. Table 5d of Peter Jenniskens (2006) lists the encounter of a filament
on August 13 at 02h UT just at the beginning of the obove mentioned interval with a possible
ZHR of about 110.
Full Moon on August 15 allow moon-free observations of the minor κ-Cygnids (012 KCG)
only after their maximum on August 18. Conditions are optimal for the Aurigids (206 AUR)
on September 1. The interesting September ε-Perseids (208 SPE) produced outbursts in2008 and 2013 reach their maximum on September 9.
In 2015, several video data sets showed low rates had persisted essentially throughout September,
identified as originating with the χ-Cygnids (757 CCY). A weak maximum was found on
September 14/15 (ZHRs about 2 or 3). The shower was also suspected in previous years, but
at a lower activity level, hence further observations would be useful, although the period is very
badly moonlit. The radiant of these very slow meteors (V∞ = 19 km/s) is at α = 300◦ , δ = +31◦ .
For convenience, we have included the radiant drift in Table 6.
Observers are encouraged to catch some Daytime Sextantids (221 DSX) in late September
to early October. There is no moonlight interference but because the radiant appears only atdawn, the twilight is the main limiting factor.
Remember that the Southern Taurids (002 STA) begin around September 10, effectively
taking over the near-ecliptic activity from the ANT through to December.
For daytime radio observers, the high activity of May-June has waned, but there remain the
γ-Leonids (203 GLE; peak due near August 25, 23h UT, albeit not found in recent radio results),
and the Sextantids (221 DSX; see page 15).
Piscis Austrinids (183 PAU)
Active: July 15–August 10; Maximum: July 28 (λ⊙ = 125◦ ); ZHR = 5;
Radiant: α = 341◦, δ = −30◦ ; Radiant drift: see Table 6;
V∞ = 35 km/s; r = 3.0.
Information of the PAU is still scarce and details on the shower are not well-confirmed. It seems
possible the ZHR may be overestimated. However, that impression could be due simply to thelarge amount of northern hemisphere summer data, and the almost complete lack of southernhemisphere winter results, on it. Observations are needed to establish and improve the listed
parameters.

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13

Southern δ-Aquariids (005 SDA)
Active: July 12–August 23; Maximum: July 30 (λ⊙ = 127◦ ); ZHR = 25;
Radiant: α = 340◦ , δ = −16◦ ; Radiant drift: see Table 6;
V∞ = 41 km/s; r = 2.5.
Radio work can pick up the SDA as well, and indeed the shower has sometimes given a surprisingly strong radio signature. Observations made by experienced observers under exceptional
observing conditions in 2008 and 2011 show that the maximum ZHR of the southern δ-Aquariids
is around 25 for about two days (λ⊙ = 125◦ − 127◦). Between λ⊙ = 124◦ and 129◦ , the ZHR
is above 20. So the shower is even more active than the Orionids. During the maximum there
are also numerous bright SDA meteors visible. This is obvious as a dip in the r-profile during
the maximum period to r ≈ 2.5 while before and after the maximum the value is much higher(r ≈ 3.1). In the past there were also outbursts observed: Australian observers reported a ZHR
of 40 in the night 1977 July 28/29; again a ZHR of 40 was observed for 1.5 hours on 2003 July
28/29 from Crete (the ZHR before and after the outburst was around 20). Unfortunately, the2003 observation was not confirmed by other observers active in the period. The extensive 2011
data set showed no ZHR enhancement at the same solar longitude as in 2003. The activity
level and variations of the shower need to be monitored. New Moon on August 1 provides optimal conditions for all of the showers in the Aquarius-Capricornus region at the end of July.
While at mid-northern latitudes only a small portion of the shower meteors is visible, conditions
significantly improve the further south the location is.

ANTα-Capricornids (001 CAP)
Active: July 3–August 15; Maximum: July 30 (λ⊙ = 127◦); ZHR = 5;
Radiant: α = 307◦ , δ = −10◦ ; Radiant drift: see Table 6;
V∞ = 23 km/s; r = 2.5.
The CAP and SDA radiants were both definitely detected visually in all years, standing out
against those much weaker ones supposed active in Capricornus-Aquarius then. Although theradiant of the CAP partly overlaps that of the large ANT region, the low CAP velocity should
allow both video and visual observers to distinguish between the two sources. Frequently, brightand at times fireball-class shower meteors are seen. Minor rate enhancements have been reported
at a few occasions in the past. The highest observed ZHR of ≈ 10 dates back to 1995. Recent
results suggest the maximum may continue into July 31.

14

IMO INFO(2-18)

Aurigids (206 AUR)
Active: August 28–September 5; Maximum: September 1, 14h UT (λ⊙ = 158 ◦. 6); ZHR = 6;
Radiant: α = 91◦ , δ = +39◦ ; Radiant drift: see Table 6;
V∞ = 66 km/s; r = 2.5.
This northern-hemisphere shower has produced short, unexpected, outbursts at times, with peak
ZHRs of ≈ 30–40 recorded in 1935, 1986 and 1994. Other events may have been missed because
the shower has not been monitored regularly until very recently. Only three observers covered
the 1986 and 1994 outbursts, for instance. The first predicted outburst happened roughly as
expected in 2007, characterized by many bright meteors. The peak ZHR of ≈ 130 lasted only
for about 20 minutes. Radio data suggested there was a ‘tail’ to that event where more faintmeteors continued for maybe an hour after the strongest peak, but visual observers could notconfirm this, probably due to the moonlit sky. The Aurigid radiant reaches a useful elevation
only after ≈ 01h local time. For 2019, there are no predictions for enhanced rates from thissource, but new Moon on September 1 guarantees perfect conditions to check.

September ε-Perseids (208 SPE)
Active: September 5–21; Maximum: September 9, 23h UT (λ⊙ = 166 ◦. 7), and possibly
September 9, 19h UT (λ⊙ = 166 ◦. 8) – see text; ZHR = 5;
Radiant: α = 48◦ , δ = +40◦ ; Radiant drift: see Table 6;
V∞ = 64 km/s; r = 3.0.
Full Moon on September 14 limits the conditions to observe this primarily northern-hemisphereshower to the ascending branch and the favourable morning hours. The radiant area is well onview all night from about 22h –23h local time for mid-northern locations. This shower produced
outbursts on 2008 September 9, between roughly λ⊙ = 166 ◦. 894–166 ◦. 921, and another brightmeteor event with a very sharp peak at λ⊙ = 167 ◦. 188 in 2013. According to Esko Lyytinen’s
modelling the next impressive SPE return may not be before 2040, and the 2019 activity should
be at the usual annual level. At the time of writing this text, a possible outburst based on
Mikiya Sato’s calculations on 2018 September 09, 19h 12m UT (λ⊙ = 166 ◦. 801) is still due.
Mikiya Sato notes that the rate on 2019 September 10, 02h 06m UT (λ⊙ = 166 ◦. 831) is probably
lower than in 2018. Since we do not yet know more about the position and extension of theassumed 1-revolution dust trail of the unknown parent object, monitoring of the activity is ofgreat importance.

IMO INFO(2-18)

15

Daytime Sextantids (221 DSX)
Active: September 9–October 9 (uncertain); Maximum: September 28 (λ⊙ = 184 ◦. 3),
Radiant: α = 152◦ , δ = 0◦ ; Radiant drift: 1◦ per day;V∞ = 32 km/s; r = 2.5 (uncertain).
Visual observers may observe some Sextantids in the pre-dawn of late September to early Octoberas part of the IMO project to collect and pool data obtained by all techniques for this shower
and the Arietids in early June. The DSX radiant is roughly 30◦ west of the Sun. Because it lies
close to the equator and the activity period is shortly after the equinox, the chances to contributeresults are almost equally good for observers in either hemisphere. As with the Arietids, both
the radiant elevation correction and the observing conditions change rapidly as morning twilightapproaches. Hence visual observers should report their data in intervals no longer than about
15–20 minutes, determining the limiting magnitude frequently during each period. The timing,and even the date, of the Sextantid maximum is uncertain. Recent radio data have indicatedthat it may occur a day earlier than expected, and it seems plausible several minor radio peaks
in early October may also be due to this source.

6

October to December

During the last quarter of the year, most of the more significant showers are observable underrather poor lunar conditions. The Draconids (009 DRA) – for which no activity peculiarities
are announced – on October 9 close to 06h UT are badly affected by a waxing gibbous Moon.
It illuminates the evening hours with a high radiant position. At mid-northern latitudes, theradiant is below 20◦ elevation after local midnight. For both, the Orionids (008 ORI) on
October 22 and the Leonis Minorids (022 LMI) on October 25 (just after last quarter Moon)
the “dark window” between radiant rise and moonlight interference is limited. This also holds
for the Leonids (013 LEO) on November 18 (waning gibbous). The best and most interesting
shower of the entire year, the Geminids (004 GEM), reaches its maximum just after fullMoon. The peak period is expected between λ⊙ = 261 ◦. 5 and λ⊙ = 262 ◦. 4 (corresponds to2019 December 14 between 02h and 23h UT). During this period, the moon is located in theconstellation Gemini only a few degrees south of the radiant. Due to the observed increase of
the peak ZHR over the last decades (Ryabova & Rendtel, 2017) observations are of interest.
Assuming a transparent sky and shielding the moonlight, an observer may still see about 20+
Geminids per hour after midnight with a high radiant position.

16

IMO INFO(2-18)

The conditions are better for the November Orionids (250 NOO) on November 28, thePhoenicids (254 PHO) on December 2, the Puppid-Velids (301 PUP) early December,the December Leonis Minorids (032 DLM) on December 20 and particularly for the Ursids(015 URS) on December 23.
The two Taurid branches dominate most of the activity from the Antihelion region in the lastquarter as described above. The ANT resume only around December 10, as the Northern
Taurids (maximum around November’s full Moon) fade away, from a radiant centre that tracks
across southern Gemini during later December, likely producing ZHRs < 2.
October Camelopardalids (281 OCT)
Active: October 5–6; Maximum: October 6, 09h 40m (λ⊙ = 192 ◦. 58); ZHR = 5(?)
Radiant: α = 164◦, δ = 79◦ ; Radiant drift: negligible;
V∞ = 47 km/s; r = 2.5 (uncertain).
Short-lived video outbursts were first recorded in 2005 and 2006 on October 5/6 (near λ⊙ 193◦)
from this north-circumpolar radiant. The shower has been detected annually (Molau et al.,2017) and produced a peak at λ⊙ = 192 ◦. 58 repeatedly with an estimated ZHR of about 5.
Enhanced activity was found last on 2016 October 5 at the predicted position at 14h 45m UT in
radio forward scatter data and video camera data from Finland.
Assuming a long-period parent, and using the 2005 outburst as reference point, Esko Lyytinen
mentions that we might see activity near λ⊙ = 192 ◦. 529 in 2018 and 2019. The return on 2018
October 6, 02h 17m UT, still has to come. The same position is reached on 2019 October 6
08h 25m UT. Surprises are possible because the stream is quite reliably a long-period case withan untypical wide 1-revolution trail or we have not yet encountered the densest part of the trail(communicated by Esko Lyytinen). Data of the 2018 return possibly shed more light on this.
Both the recurrent maximum given in the box and the calculated position are favourable forobservers at (North) American longitudes. The first quarter Moon mainly disturbs the evening
hours.

OCT
Oct 06

IMO INFO(2-18)

17

Southern Taurids (002 STA)
Active: September 10–November 20; Maximum: October 10 (λ⊙ = 197◦ ); ZHR = 5;
Radiant: α = 32◦ , δ = +09◦; Radiant drift: see Table 6;
V∞ = 27 km/s; r = 2.3.
This stream, with its Northern counterpart, forms part of the complex associated with Comet
2P/Encke. For shower association, assume the radiant to be an oval area, extending about 20◦
in α and about 10◦ in δ, centred on the radiant position for any given date. The Taurid activity
overall dominates the Antihelion Source area’s during the northern autumn, so much so that
the ANT is considered inactive while either branch of the Taurids is present. The brightness
and relative slowness of many Taurid meteors makes them ideal targets for still-imaging, whilethese factors coupled with low, steady, Taurid rates makes them excellent subjects to practicevisual plotting techniques on. Although long thought to combine with the Northern Taurids to
produce an apparently plateau-like maximum in the first decade of November, VID and visualplotting work have indicated the Southern branch reaches its peak about a month before theNorthern one, this year only shortly before October’s full Moon. Its near-ecliptic radiant means
all meteoricists can observe the STA, albeit northern hemisphere observers are somewhat betterplaced, as here suitable radiant elevations persist for much of the night. Even in the southernhemisphere however, 3–5 hours’ watching around local midnight is possible with Taurus wellclear of the horizon.

α-Monocerotids (246 AMO)
Active: November 15–25; Maximum: November 22, 06h UT (λ⊙ = 239 ◦. 32);
ZHR = variable, usually ≈ 5, but has produced an outburst to ≈ 400, see text;
Radiant: α = 117◦ , δ = +01◦ ; Radiant drift: see Table 6;
V∞ = 65 km/s; r = 2.4.
The most recent α-Monocerotid outburst was observed in 1995. The peak ZHR of ≈ 420 lasted
for just five minutes, the entire outburst 30 minutes. Recent modelling by Esko Lyytinen has
indicated the main AMO trail crosses the Earth’s orbit in 2017 and 2020. However, the Earth is
not near those points in November, so no strong outburst is likely to happen then. A weak return
may occur in November 2019, ahead of the 2020 encounter, depending on how broad the trail

18

IMO INFO(2-18)

may be. The next strong AMO outburst is unlikely before 2043. Mikiya Sato’s modelling hints
at a possible dust trail approach at λ⊙ = 239 ◦. 310 (2019 November 22, 04h 56m UT) – perhaps
the highest rate in the 2016–2019 interval. The same trail encounter (classified as “far”) is listed
in Table 3 of Peter Jenniskens’ (2006) book (λ⊙ = 239 ◦. 306; 2019 November 22, 04h 52m UT).

Seen the small activity mainly found in radio data close to the positions expected to Mikiya Sato’s
previous calculations in 2016 and 2017, observers are advised to monitor the AMO annually. The
brevity of all past outbursts means breaks under clear skies should be kept to a minimum near
the predicted peak. The waning Moon (last quarter on the 18th) should allow useful observations
when the shower’s radiant is well on view from either hemisphere after about 23h local time.
November Orionids (250 NOO)
Active: November 14–December 6; Maximum: November 28 (λ⊙ = 246◦ ); ZHR = 3;
Radiant: α = 91◦ , δ = +16◦ ; Radiant drift: see Table 6;
V∞ = 41 km/s; r = 3.0.

NOO
Dec 0525

Nov 15

Detailed analysis of video data revealed that there are two consecutive, very similar showers
whose activity intervals overlap by only two degrees in solar longitude: the November Orionids(250 NOO), followed by the Monocerotids (019 MON). In the last days of November the shower

IMO INFO(2-18)

19

is the strongest source in the sky. The radiant is located in northern Orion, 4◦ north of αOrionis. This location is close to the Northern Taurids, but far enough east to distinguishmeteors from the two sources. Additionally, the faster velocity of the November Orionids should
help distinguish these meteors from the slower Taurids. The radiant culminates near 2h local
time, but is above the horizon for most of the night. New Moon on November 26 offers best
circumstances to collect data.
Phoenicids (254 PHO)
Active: November 22–December 9; Maximum: December 2, 19h UT (λ⊙ = 250 ◦. 0);
ZHR = variable, usually none, see text;
Radiant: α = 18◦ , δ = −53◦ ; Radiant drift: see Table 6;
V∞ = 18 km/s; r = 2.8.
Only one impressive Phoenicid return has been reported, that of its discovery in 1956, when thepeak ZHR probably reached ≈ 100, possibly with several peaks spread over a few hours. Recent
significant activity was observed on 2014 December 1. This was predicted by Sato and Watanabe(2010). In the same paper, several encounters with dust trails are calculated for the 2019 return.
The Earth comes closest to the 1898 dust trail at λ⊙ = 250 ◦. 132 (2019 December 2, 21h 29m ).
The estimated ZHR may reach 12. A weaker trail may be encountered at λ⊙ = 240 ◦. 140 alreadyon November 23, 00h 39m
As the dates are around new Moon (November 26), observers should check for possible Phoenicids
throughout the entire period given above. From the southern hemisphere (only), the Phoenicid radiant culminates at dusk, remaining well on view for most of the night. Phoenicids are
extremely slow meteors.

Puppid-Velids (301 PUP)
Active: December 1–15; Maximum: December ≈ 7 (λ⊙ ≈ 255◦ ); ZHR ≈ 10;
Radiant: α = 123◦ , δ = −45◦ ; Radiant drift: see Table 6;
V∞ = 40 km/s; r = 2.9.
This is a complex system of poorly-studied showers, visible chiefly from locations south of theequator. Several sub-streams have been proposed (301 PUP representing an “average” position),with radiants so tightly clustered, visual observing cannot readily separate them. The activity
is poorly-established, though the higher rates seem to occur in early to mid December, with a20

IMO INFO(2-18)

waxing Moon this year (first quarter on December 4). Some PUP activity may be visible prior
and after the given period. Occasional bright fireballs, notably around the suggested maximum,
have been reported regularly. The radiant area is on-view all night, highest towards dawn.

Monocerotids (019 MON)
Active: November 27–December 17; Maximum: December 9 (λ⊙ = 257◦); ZHR = 3;
Radiant: α = 100◦, δ = +08◦ ; Radiant drift: see Table 6;
V∞ = 42 km/s; r = 3.0.
This very minor shower’s details need further improvement by observational data. Visual data
give a maximum of ZHR 2–3 at λ⊙ ≈ 257◦ . Video data (2011–2016) show a peak at λ⊙ ≈ 262 ◦. 0◦(i.e. December 14) with a ZHR of the order of 8 coinciding with the Geminid peak. Care needs
to be taken to clearly distinguish MON from GEM. Visual observers should choose their field ofview such, that the radiants do not line up. (Field centres near Taurus in the evening or near Leo
in the morning are possible choices.) December’s new Moon period creates perfect conditions
for either potential maximum timing, as the radiant area is available virtually all night for muchof the globe, culminating at about 01h 30m local time.

IMO INFO(2-18)

21

Ursids (015 URS)
Active: December 17–26; Maximum: December 23, 03h UT (λ⊙ = 270 ◦. 7);
ZHR = 10 (occasionally variable up to 50);
Radiant: α = 217◦ , δ = +76◦ ; Radiant drift: see Table 6;
V∞ = 33 km/s; r = 2.8.

A poorly-observed northern hemisphere shower, but one which has produced at least two major
outbursts in the past ≈ 70 years, in 1945 and 1986. Several lesser rate enhancements havebeen reported as well, most recently from 2006–2008, which were possibly influenced by the
relative proximity of the shower’s parent comet, 8P/Tuttle, last at perihelion on 2008 January
27. Slightly enhanced rates have also been reported in 2011 and 2014. Other events could
have been missed easily. For 2019, an encounter of an Ursid filament is announced by Peter
Jenniskens (2006; Table 5b) at λ⊙ = 270 ◦. 49 (2019 December 22, 21h39m ) with a possible ZHRof the order of 30. At this time, there is rather little interference by the waning Moon (lastquarter on December 19). Recent data analyses have shown that the population index is rather
r = 2.2 around the maximum, i.e. the portion of slightly brighter shower meteors is higher thanin the outer sections of the shower, although the Ursids are not known for fireball events. The
Ursid radiant is circumpolar from most northern sites, while the shower is not observable frommost southern locations. The radiant culminates after daybreak, and is highest in the sky after
midnight.

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IMO INFO(2-18)

7

Radiant sizes and meteor plotting for visual observers

by Rainer Arlt
If you are not observing during a major-shower maximum, it is essential to associate meteors with
their radiants correctly, since the total number of meteors will be small for each source. Meteor
plotting allows shower association by more objective criteria after your observation than thesimple imaginary back-prolongation of paths under the sky. With meteors plotted on gnomonic
maps, you can trace them back to their radiants by extending their straight line paths. If aradiant lies on another chart, you should find common stars on an adjacent chart to extend thisback-prolongation correctly.
How large a radiant should be assumed for shower association? The real physical radiant size isvery small, but visual plotting errors cause many true shower meteors to miss this real radiantarea. Thus we have to assume a larger effective radiant to allow for these errors. Unfortunately,
as we enlarge the radiant, so more and more sporadic meteors will appear to line up accidentallywith this region. Hence we have to apply an optimum radiant diameter to compensate for theplotting errors loss, but which will not then be swamped by sporadic meteor pollution. Table 1
gives this optimum diameter as a function of the distance of the meteor from the radiant.

Table 1. Optimum radiant diameters to be assumed forshower association of minor-shower meteors as a function of
the radiant distance D of the meteor.
D
15◦
30◦
50◦
70◦

optimum diameter
14◦
17◦
20◦
23◦

Note that this radiant diameter criterion applies to all shower radiants except those of theSouthern and Northern Taurids, and the Antihelion Source, all of which have notably larger
radiant areas. The optimum α × δ size to be assumed for each radiant of the two Taurid showers
is instead 20◦ × 10◦ , while that for the Antihelion Source is still larger, at 30◦ × 15◦ .
Path-direction is not the only criterion for shower association. The angular velocity of the meteor
should match the expected speed of the given shower meteors according to their geocentric
velocities. Angular velocity estimates should be made in degrees per second (◦ /s). To do this,make the meteors you see move for one second in your imagination at the speed you saw them.
The path length of this imaginary meteor is the angular velocity in ◦ /s. Note that typical speeds
are in the range 3◦ /s to 25◦ /s. Typical errors for such estimates are given in Table 2.
Table 2. Error limits for the angular velocity.
angular velocity [◦ /s]
permitted error [◦ /s]

5
3

10 15 20 30
5 6 7 8

If you find a meteor in your plots which passes the radiant within the diameter given by Table 1,
check its angular velocity. Table 3 gives the angular speeds for a few geocentric velocities, which
can then be looked up in Table 5 for each shower.

IMO INFO(2-18)

23

Table 3. Angular velocities as a function of the radiant distance of the meteor (D) and theelevation of the meteor above the horizon (h) for three different geocentric velocities (V∞ ). All
velocities are in ◦ /s.
h\D

10◦

V∞ = 25 km/s
20◦ 40◦ 60◦ 90◦

10◦

20◦

10◦
20◦
40◦
60◦
90◦

0.4
0.9
1.6
2.2
2.5

0.9
1.7
3.2
4.3
4.9

0.7
1.4
2.6
3.5
4.0

1.4
2.7
5.0
6.8
7.9

8

1.6
3.2
5.9
8.0
9.3

2.2
4.3
8.0
11
13

2.5
4.9
9.3
13
14

V∞ = 40 km/s
40◦ 60◦ 90◦
2.6
5.0
9.5
13
15

3.5
6.8
13
17
20

4.0
7.9
15
20
23

10◦

V∞ = 60 km/s
20◦ 40◦ 60◦ 90◦

0.9
1.8
3.7
4.6
5.3

1.8
3.5
6.7
9.0
10

Tables: lunar and shower data
Table 4. Lunar phases for 2019.
New MoonFirst Quarter

Full Moon

Last Quarter

January 6
February 4
March 6
April 5May 4
June 3
July 2
August 1
August 30
September 28
October 28
November 26
December 26

January 14
February 12
March 14
April 12
May 12June 10
July 9August 7
September 6
October 5
November 4
December 4

January 21
February 19
March 21
April 19
May 18June 17
July 16
August 15
September 14
October 13
November 12
December 12

January 27
February 26
March 28
April 26
May 26
June 25
July 25
August 23
September 22
October 21
November 19
December 19

3.7
6.7
13
17
20

4.6
9.0
17
23
26

5.3
10
20
26
30

24

IMO INFO(2-18)

Table 5. Working List of Visual Meteor Showers. Details in this Table were correct
according to the best information available in June 2018, with maximum dates accurate only
for 2019. The parenthesized maximum date for the Puppids-Velids indicates a reference date
for the radiant only, not necessarily a true maximum. Some showers have ZHRs that vary fromyear to year. The most recent reliable figure is given here, except for possibly periodic showers
which are noted as ‘Var’ = variable. For more information check the updates published e.g. in
the IMO Journal WGN.
ShowerAntihelion Source (ANT)

Activity

MaximumDateλ⊙Radiant
α
δ

V∞
km/s

r

ZHR

Dec 10–Sep 10–

March–April,late May, late June

see Table 6

30

3.0

4

230◦
228◦
210◦
239◦
271◦
110◦
338◦
287◦
44◦
224◦
341◦
340◦
307◦
48◦
286◦
91◦
48◦
152◦
164◦
262◦
32◦
84◦
102◦
95◦
162◦
58◦
152◦
117◦
91◦
18◦
123◦
100◦
127◦
112◦
175◦
161◦
217◦

41
31
58
56
49
18
66
43
38
18
35
41
23
59
25
66
64
32
47
20
27
64
70
66
62
29
71
65
44
18
40
41
58
35
65
64
33

2.1
3.0
2.0
2.4
2.1
2.0
2.4
3.0
2.8
2.2
3.0
2.5
2.5
2.2
3.0
2.5
3.0
2.5
2.5
2.6
2.3
3.0
3.0
2.5
3.0
2.3
2.5
2.4
3.0
2.8
2.9
3.0
3.0
2.6
3.0
3.0
2.8

110
3
6
6
18
Var
50
3
30
Var
5
25
5
110
3
6
5
5
5
10
5
2
3
20
2
5
15
Var
3
Var
10
2
3
140
3
5
10

Quadrantids (010 QUA)
Dec 28–Jan 12
γ-Ursae Minorids (404 GUM) Jan 10–Jan 22
α-Centaurids (102 ACE)
Jan 31–Feb 20
γ-Normids (118 GNO)
Feb 25–Mar 28
Lyrids (006 LYR)
Apr 14–Apr 30
π-Puppids (137 PPU)
Apr 15–Apr 28
η-Aquariids (031 ETA)
Apr 19–May 28
η-Lyrids (145 ELY)
May 03–May 14
Dayt. Arietids (171 ARI) May 14–Jun 24
June Bootids (170 JBO) Jun 22–Jul 02
Piscis Austr. (183 PAU)
Jul 15–Aug 10
S. δ-Aquariids (005 SDA) Jul 12–Aug 23
α-Capricornids (001 CAP) Jul 03–Aug 15
Perseids (007 PER)
Jul 17–Aug 24
κ-Cygnids (012 KCG)
Aug 03–Aug 25
Aurigids (206 AUR)
Aug 28–Sep 05
Sep. ε-Perseids (208 SPE) Sep 05–Sep 21
Dayt. Sextantids (221 DSX) Sep 09–Oct 09
Oct. Camelopard. (281 OCT) Oct 05–Oct 06
Draconids (009 DRA)
Oct 06–Oct 10
S. Taurids (002 STA)
Sep 10–Nov 20
δ-Aurigids (224 DAU)
Oct 10–Oct 18
ε-Geminids (023 EGE)
Oct 14–Oct 27
Orionids (008 ORI)
Oct 02–Nov 07
Leonis Minorids (022 LMI) Oct 19–Oct 27
N. Taurids (017 NTA)Oct 20–Dec 10
Leonids (013 LEO)
Nov 06–Nov 30
α-Monocerotids (246 AMO) Nov 15–Nov 25
Nov. Orionids (250 NOO) Nov 13–Dec 06
Phoenicids (254 PHO)
Nov 22–Dec 09
Puppid-Velids (301 PUP) Dec 01–Dec 15
Monocerotids (019 MON) Dec 05–Dec 20
σ-Hydrids (016 HYD)
Dec 03–Dec 15
Geminids (004 GEM)
Dec 04–Dec 17
Comae Berenic. (020 COM) Dec 12–Dec 23
Dec. Leonis Min. (032 DLM) Dec 05–Feb 04
Ursids (015 URS)
Dec 17–Dec 26

Jan 04
Jan 18
Feb 08Mar 15
Apr 23
Apr 24
May 06
May 09Jun 08Jun 27
Jul 28
Jul 30Jul 30Aug 13
Aug 18
Sep 01
Sep 09Sep 28
Oct 06
Oct 09Oct 10
Oct 11
Oct 19Oct 22
Oct 25
Nov 13
Nov 18
Nov 22
Nov 28
Dec 02(Dec 07)
Dec 09Dec 12
Dec 14
Dec 16
Dec 20Dec 23283 ◦. 16298◦
319 ◦. 2354◦
32 ◦. 32
33 ◦. 545 ◦. 548 ◦. 076 ◦. 695 ◦. 7
125◦
127◦
127◦
140 ◦. 0145◦
158 ◦. 6
166 ◦. 7
184 ◦. 3
192 ◦. 58
195 ◦. 4
197◦
198◦
205◦
208◦
211◦
230◦
235 ◦. 27
239 ◦. 32
246◦
250 ◦. 0(255◦ )
257◦
260◦
262 ◦. 2264◦268◦
270 ◦. 7

Table 6 (next page). Radiant positions during the year in α and δ.

+49◦
+67◦
−59◦
−50◦
+34◦
−45◦
−01◦
+44◦
+24◦
+48◦
−30◦
−16◦
−10◦
+58◦
+59◦
+39◦
+40◦
+00◦
+79◦
+54◦
+09◦
+44◦
+27◦
+16◦
+37◦
+22◦
+22◦
+01◦
+16◦
−53◦
−45◦
+08◦
+02◦
+33◦
+18◦
+30◦
+76◦

IMO INFO(2-18)
Date
Jan
0
Jan
5
Jan
10
Jan
15
Jan
20
Jan
25
Jan
30
Feb
5
Feb
10
Feb
15
Feb
20
Feb
28
Mar
5
Mar 10Mar 15
Mar 20Mar 25
Mar 30
Apr
5
Apr 10
Apr 15
Apr 20
Apr 25
Apr 30
May 05
May 10
May 15
May 20
May 25
May 30Jun
5
Jun 10Jun 15
Jun 20Jun 25
Jun 30
Jul
5
Jul
10
Jul
15
Jul
20
Jul
25
Jul
30
Aug
5
Aug 10Aug 15
Aug 20Aug 25
Aug 30
Sep
5
Sep
10
Sep
15
Sep
20
Sep
25
Sep
30
Oct
5
Oct
10
Oct
15
Oct
20
Oct
25
Oct
30
Nov
5
Nov 10
Nov 15
Nov 20
Nov 25
Nov 30
Dec
5
Dec 10Dec 15
Dec 20Dec 25
Dec 30ANT112◦ +21◦117◦ +20◦
122◦ +19◦127◦ +17◦132◦ +16◦138◦ +15◦143◦ +13◦149◦ +11◦
154◦
+9◦
◦
159
+7◦
164◦
+5◦
◦
172
+2◦
◦
177
0◦
182◦
−2◦
187◦
−4◦
192◦
−6◦
◦
197
−7◦
◦
202
−9◦
208◦ −11◦213◦ −13◦218◦ −15◦222◦ −16◦227◦ −18◦232◦ −19◦237◦ −20◦242◦ −21◦247◦ −22◦252◦ −22◦256◦ −23◦262◦ −23◦267◦ −23◦272◦ −23◦276◦ −23◦281◦ −23◦286◦ −22◦291◦ −21◦296◦ −20◦300◦ −19◦305◦ −18◦
310◦ −17◦315◦ −15◦319◦ −14◦325◦ −12◦330◦ −10◦
335◦
−8◦
◦
340
−7◦
344◦
−5◦
349◦
−3◦
◦
355
−1◦
0◦
+1◦

EGE
99◦ +27◦104◦ +27◦109◦ +27◦
NOO
81◦ +16◦84◦ +16◦88◦ +16◦92◦ +16◦85◦ +23◦90◦ +23◦96◦ +23◦101◦ +23◦106◦ +22◦111◦ +21◦
ANT

25
QUA
228◦ +50◦
231◦ +49◦234◦ +48◦

DLM
172◦ +25◦176◦ +23◦180◦ +21◦185◦ +19◦189◦ +17◦193◦ +15◦
198◦ +12◦203◦ +10◦

GNO
225◦ −51◦
230◦ −50◦
235◦ −50◦240◦ −50◦245◦ −49◦250◦ −49◦255◦ −49◦
LYR
263◦ +34◦269◦ +34◦274◦ +34◦279◦ +34◦

PPU106◦ −44◦109◦ −45◦111◦ −45◦ACE200◦ −57◦
208◦ −59◦214◦ −60◦
220◦ −62◦225◦ −63◦

ETA
323◦
−7◦
◦
328
−5◦
332◦
−3◦
◦
337
−1◦
◦
341
+1◦
345◦
+3◦
◦
349
+5◦
353◦
+7◦

GUM
220◦ +71◦224◦ +69◦
228◦ +67◦
232◦ +65◦ELY283◦ +44◦288◦ +44◦293◦ +45◦

ARI
42◦ +24◦47◦ +24◦
JBO
223◦ +48◦
225◦ +47◦
PER6◦ +50◦11◦ +52◦
22◦ +53◦29◦ +54◦37◦ +56◦45◦ +57◦
51◦ +58◦
57◦ +58◦
63◦ +58◦
STA
12◦
+3◦
◦
15
+4◦
◦
18
+5◦
21◦
+6◦
◦
25
+7◦
28◦
+8◦
◦
32
+9◦
◦
36
+11◦
40◦ +12◦43◦ +13◦47◦ +14◦52◦ +15◦56◦ +15◦60◦ +16◦64◦ +16◦
GEM
103◦ +33◦
108◦ +33◦
113◦ +33◦
118◦ +32◦
QUA
226◦ +50◦

CAP285◦ −16◦289◦ −15◦294◦ −14◦299◦ −12◦303◦ −11◦307◦ −10◦
313◦
−8◦
◦
318
−6◦
AUR
85◦ +40◦90◦ +39◦96◦ +39◦102◦ +39◦
DSX
150◦
0◦
◦
155
0◦
NTA
38◦ +18◦43◦ +19◦47◦ +20◦52◦ +21◦56◦ +22◦61◦ +23◦65◦ +24◦70◦ +24◦74◦ +24◦149◦ +37◦
153◦ +35◦
157◦ +33◦
161◦ +31◦
166◦ +28◦170◦ +26◦
DLM

SDA
325◦ −19◦329◦ −19◦333◦ −18◦337◦ −17◦340◦ −16◦345◦ −14◦349◦ −13◦352◦ −12◦356◦ −11◦SPE
43◦ +40◦48◦ +40◦53◦ +40◦59◦ +41◦
ORI
85◦ +14◦88◦ +15◦91◦ +15◦94◦ +16◦98◦ +16◦101◦ +16◦105◦ +17◦
PHO
10◦ −52◦14◦ −52◦18◦ −53◦22◦ −53◦174◦ +19◦177◦ +18◦180◦ +16◦
COM

PAU
330◦
−34
334◦
−33
338◦
−31
343◦
−29
348◦
−27
352◦
−26

CCY
293◦ +29◦297◦ +30◦301◦ +31◦305◦ +32◦309◦ +33◦
DAU
82◦ +45◦87◦ +43◦92◦ +41◦
LEO
147◦ +24◦150◦ +23◦153◦ +21◦156◦ +20◦
159◦ +19◦
122◦
+3◦
126◦
+2◦
◦
130
+1◦
HYD

KCG
283◦ +58◦284◦ +58◦285◦ +59◦286◦ +59◦288◦ +60◦
289◦ +60◦

OCT164◦ +79◦

DRA262◦ +54◦

LMI
158◦ +39◦163◦ +37◦168◦ +35◦

PUP
120◦ −45◦122◦ −45◦125◦ −45◦128◦ −45◦217◦ +76◦
217◦ +74◦
URS

AMO
112◦
+2◦
◦
116
+1◦
120◦
0◦
91◦
+8◦
98◦
+9◦
101◦
+8◦
105◦
+7◦
◦
108
+7◦
MON

26

IMO INFO(2-18)

Table 7. Working List of Daytime Radio Meteor Showers. According to the naming rules, theshower names should all have ‘Daytime’ added (it is omitted in this Table). An asterisk (‘*’) in the‘Max date’ column indicates that source may have additional peak times, as noted in the text above.
See also the details given for the Arietids (171 ARI) and the Sextantids (221 DSX) in the text part of
the Calendar. Rates are expected to be low (L), medium (M) or high (H). An asterisk in the ‘Rate’column shows the suggested rate may not recur in all years. (Thanks to Jean-Louis Rault and Cis
Verbeeck for comments on the Table.)
ShowerCapricornids/Sagittariids (115 DCS)
χ-Capricornids (114 DXC)
April Piscids (144 APS)
ε-Arietids (154 DEA)May Arietids (294 DMA)
o-Cetids (293 DCE)
Arietids (171 ARI)
ζ-Perseids (172 ZPE)
β-Taurids (173 BTA)
γ-Leonids (203 GLE)
Daytime Sextantids (221 DSX)

Activity

Max.
Date

λ⊙
2000

RadiantαδRate

Jan 13–Feb 04
Jan 29–Feb 28
Apr 20–Apr 26
Apr 24–May 27
May 04–Jun 06
May 05–Jun 02
May 14–Jun 24
May 20–Jul 05
Jun 05–Jul 17
Aug 14–Sep 12
Sep 09–Oct 09

Feb 01∗
Feb 13∗
Apr 22
May 09May 16
May 20
Jun 07
Jun 09∗Jun 28Aug 25
Sep 27∗312 ◦. 5324 ◦. 7
32 ◦. 548 ◦. 755 ◦. 559 ◦. 376 ◦. 678 ◦. 696 ◦. 7152 ◦. 2
184 ◦. 3

299◦
315◦
9◦
44◦
37◦
28◦
42◦
62◦
86◦
155◦
152◦

M∗
L∗
L
L
L
M∗
H
H
M
L∗
M∗

−15◦
−24◦
+11◦
+21◦
+18◦
−04◦
+25◦
+23◦
+19◦
+20◦
0◦

IMO INFO(2-18)

927

References and Abbreviations

References:
Jenniskens P., 2006: Meteor showers and their parent comets. Cambridge Univ. Press
Molau S., Crivello S., Goncalves R., Saraiva C., Stomeo E., Kac J., 2016a: Results of the IMO
Video Meteor Network – February 2016, WGN 44, pp. 116–119.
Molau S., Crivello S., Goncalves R., Saraiva C., Stomeo E., Kac J., 2016b: Results of the IMO
Video Meteor Network – July 2016, WGN 44, pp. 205–210.
Molau S., Crivello S., Goncalves R., Saraiva C., Stomeo E., Kac J., 2017: Results of the IMO
Video Meteor Network – October 2016, WGN 45, pp. 39–42.
Molau S., Rendtel J., 2009: A comprehensive list of meteor showers obtained from 10 years ofobservations with the IMO Video Meteor Network, WGN 37:4, pp. 98–121
Ryabova G., Rendtel J., 2017: Increasing Geminid meteor shower activity, Monthly Notices
Royal astron. Soc. Lett. 475, pp. L77–L80.
Sato M., Watanabe J., 2010: Forecast for Phoenicids in 2008, 2014, and 2019, Publ. Astron.
Soc. Japan 62, pp. 509–513.

Abbreviations:• α, δ: Coordinates for a shower’s radiant position, usually at maximum. α is right ascension,δ is declination. Radiants drift across the sky each day due to the Earth’s own orbital
motion around the Sun, and this must be allowed for using the details in Table 6 for nights
away from the listed shower maxima.
• r: The population index, a term computed from each shower’s meteor magnitude distribution. r = 2.0–2.5 implies a larger fraction of brighter meteors than average, while r above
3.0 is richer in fainter meteors than average.
• λ⊙ : Solar longitude, a precise measure of the Earth’s position on its orbit which is notdependent on the vagaries of the calendar. All λ⊙ are given for the equinox 2000.0.
• V∞ : Pre-atmospheric or apparent meteoric velocity, given in km/s. Velocities range fromabout 11 km/s (very slow) to 72 km/s (very fast). 40 km/s is roughly medium speed.
• ZHR: Zenithal Hourly Rate, a calculated maximum number of meteors an ideal observer
would see in perfectly clear skies (reference limiting magnitude +6.5) with the shower
radiant overhead. This figure is given in terms of meteors per hour.

28

10

IMO INFO(2-18)

Useful addresses

On the IMO’s website http://www.imo.net you find online forms to submit visual reports andreports of fireball sightings. It is also possible to submit reports of visual observation sessions
for other observers. You can also access all reports in the database, both of visual data andfireball reports.
Visual reports: http://www.imo.net → Observations → Add a visual observation session
Fireball reports: http://www.imo.net → Observations → Report a fireballFor more information on observing techniques, to see the latest results from well-observed major
meteor showers and unusual shower outbursts, or when you wish to submit your results, please
use the IMO’s website, www.imo.net as your first stop. The web page also allows to accessthe data for own analyses. Questions can be mailed to the appropriate address (note the word
“meteor” must feature in your message’s “subject” line to pass the anti-spam filters):
For especially bright meteors: fireball@imo.net
For meteor still imaging: photo@imo.net
For forward-scatter radio observing: radio@imo.net
For meteor moving-imaging: video@imo.net
For visual observing: visual@imo.net
The IMO has Commssions for various fields, about which you may enquire with the respective
director:
Photographic Commission: William Ward, School of Engineering, Rankine Building, Oakfield Avenue, Glasgow G12 8LT, Scotland, U.K.; e-mail: William.Ward@glasgow.ac.uk
Radio Commission: Jean-Louis Rault, Société Astronomique de France, 16 Rue de la Valleé,F-91360 Epinay sur Orge, France; e-mail: f6agr@orange.fr
Video Commission Sirko Molau, Abenstalstraße 13b, D-84072 Seysdorf, Germany;e-mail: sirko@molau.deVisual Commission: Rainer Arlt, Leibniz-Institut f. Astrophysik, An der Sternwarte 16,
D-14482 Potsdam, Germany; e-mail: rarlt@aip.de
You can join the International Meteor Organization by visiting the web page www.imo.net →“Join the IMO”.
As an alternative or to obtain additional information, you may contact the Secretary-General
via lunro.imo.usa@cox.net.
Those unable to access the Internet may write for information to Robert Lunsford, IMO SecretaryGeneral, 14884 Quail Valley Way, El Cajon, CA 92021-2227, USA. When using ordinary mail,please try to enclose return postage, either in the form of stamps (same country only) or as an
International Reply Coupon (I.R.C. – available from main postal outlets). Thank you!

c International Meteor Organization, 2018.