主要流星雨月相参考http://tianxiangyubao.happymm.cn/script/forum/view.asp?article_id=783476
1.Quadrantids (QUA)1月4日15时20分象限仪座流星雨极大（通常120颗，但有时可能会有60到200颗，不过今年受月光较强）
  由IMCCE提供的流星体轨道数据图2012

 

 

 

Active: December 28 — January 12; Maximum: January 4, 07h20m 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; TFC: α = 242°, δ = +75° and α = 198°, δ = +40° (β > 40° N). IFC: before 0h local time α = 150°, δ = +70°; after 0h local time α = 180°, δ = +40° and α = 240°, δ = +70° (β > 40° N).

http://www.imo.net/galleries/calendar/img/QUA.jpg

Waxing gibbous moonset for the predicted Quadrantid maximum leaves several dark-sky hours for visual observing before morning twilight begins from northern hemisphere sites this year. From many such places, the shower's radiant is circumpolar, in northern Boötes, first attaining a useful elevation after local midnight, improving steadily later, making this a reasonably favourable return. Observing sites from eastern North America east to the extreme west of Europe should be best-placed to record what happens, if the maximum time above is correct.

Modelling the stream is difficult. While the graph shown in HMO p. 129, based on computations by Jérémie Vaubaillon, seemed to suggest enhanced rates could happen between roughly 01^h to 10^h UT on January 4, his recent results do not support this. The λ⊙ = 283.16° maximum timing is based on the best-observed return of the shower ever analysed, from IMO data collected in 1992, as confirmed by radio results in most years since 1996. The peak itself is normally short-lived, and can be easily missed in just a few hours of poor northern-winter weather, which may be why the ZHR level apparently fluctuates from year to year. However, some genuine variability is probably present too. An added level of complexity comes from the fact mass-sorting of particles across the meteoroid stream may make fainter objects (radio and telescopic meteors) reach maximum up to 14 hours before the brighter (visual and photographic) ones, so observers should be alert throughout the shower. A few years since 2000 seem to have produced a, primarily radio, maximum following the main visual one by some 9—12 hours. Visual confirmation of any repeat of such behaviour would be welcomed. QUA activity tends to be very low more than a day or so from the peak, and past observations have suggested the radiant is diffuse away from the maximum too, contracting notably during the peak itself, perhaps because of this lower activity then. Imaging observations would be welcomed to help investigate this topic, along with telescopic results.
 

2.Lyrids (LYR)4月22日13时30分天琴座流星雨极大（通常18颗，但有可能90颗，要看运气了）

 由爱尔兰阿马山天文台提供的数据图2012

 

 

 

Active: April 16—25; Maximum: April 22, 05h30m UT (λ⊙ = 32.32°), but may vary — see text; ZHR = 18 (can be variable, up to 90); Radiant: α = 271°, δ = +34°; Radiant drift: see Table 6; V∞ = 49 km/s; r = 2.1; TFC: α = 262°, δ = +16° and α = 282°, δ = +19° (β > 10° S).

http://www.imo.net/galleries/calendar/img/LYR.jpg

The λ⊙ = 32.32° timing given above is the 'ideal' maximum found in IMO results from 1988—2000. However, the maximum time was variable from year to year between λ⊙ = 32.0°—32.45° (equivalent to 2012 April 21, 21^h30^m to April 22, 08^h30^m UT). Activity was variable too. A peak at the ideal time produced the highest ZHRs, ∼ 23, while the further the peak happened from this, the lower the ZHRs were, down to ∼ 14. (The last very high maximum was in 1982, when a shortlived ZHR of 90 was recorded.) The mean peak ZHR was 18 over the thirteen years examined.

While generally thought of as having a short, quite sharp, maximum, this investigation showed the shower's peak length was inconstant. Using the Full-Width-Half-Maximum time (the period ZHRs were above half the peak level), a variation between 14.8 to 61.7 hours was detected (mean 32.1 hours). The best rates are normally achieved for just a few hours even so. The analysis also confirmed that occasionally, as their highest rates occurred, the Lyrids produced a brief increase in fainter meteors. Lyrids are best viewed from the northern hemisphere, but are visible from many sites north and south of the equator. As the radiant rises during the night, watches can be carried out usefully after about 22^h30^m local time from mid-northern sites, but only well after midnight from the mid-southern hemisphere. New Moon on April 21 makes this year perfect for Lyrid maximum observing, and if the ideal peak time recurs, it should be best-seen from sites across much of North America, particularly the eastern half. Remember, other maximum times are perfectly possible!
 

3.π-Puppids (PPU)船尾座π流星雨（今年极大值在4月23日18时30分，极大值流量在40颗左右每小时）

 由爱尔兰阿马山天文台提供的数据图2012

 

Active: April 15—28; Maximum: April 23, 10h30m UT (λ⊙ = 33.5°); ZHR = periodic, up to around 40; Radiant: α = 110°, δ = –45°; Radiant drift: see Table 6; V∞ = 18 km/s; r = 2.0; TFC: α = 135°, δ = –55° and α = 105°, δ = –25° (β < 20° N).

http://www.imo.net/galleries/calendar/img/PPU.jpg

Activity has only been detected from this source since 1972, with notable, short-lived, shower maxima of around 40 meteors per hour in 1977 and 1982, both years when its parent comet, 26P/Grigg-Skjellerup was at perihelion. Before 1982, little activity had been seen at other times, but in 1983, a ZHR of ∼ 13 was reported, perhaps suggesting material has begun to spread further along the comet's orbit, as theory predicts. Comet Grigg-Skjellerup's most recent perihelion in 2008 March produced nothing meteorically significant that April, but lunar circumstances in 2008 were poor, and faint-meteor activity (which was predicted as likely in advance) could have been missed. There were no predictions for activity in 2012 when this Calendar was prepared. The π–Puppids are best-seen from the southern hemisphere, with useful observations mainly practical there before midnight, as the radiant is very low to setting after 01^h local time. April's new Moon creates perfect viewing circumstances this year.

Covering whatever happens is important, even if that is to report no obvious activity, as past datasets on the shower have typically been very patchy. So far, visual and radio data have been collected on the shower, but the slow, sometimes bright nature of the meteors makes them ideal subjects for imaging too. No telescopic or video data have been reported in any detail as yet.

 

4.June Boötids (JBO)6月27日11时六月牧夫座流星雨极大，变化0到100颗每小时之间，看运气

 由IMCCE提供的流星体轨道数据图2012

 由爱尔兰阿马山天文台提供的数据2012

 

 

Active: June 22 — July 2; Maximum: June 27, 03h 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; TFC: α = 156°, δ = +64° and α = 289°, δ = +67° (β = 25°—60° N).

http://www.imo.net/galleries/calendar/img/JBO.jpg

This source was reinstated on the Working List after its unexpected return of 1998, when ZHRs of 50—100+ were visible for more than half a day. Another outburst of similar length, but with ZHRs of ∼ 20—50 was observed on 2004 June 23, a date before definite activity had previously been recorded from this shower.

Consequently, the shower's start date was altered to try to ensure future activity so early is caught, and we encourage all observers to routinely monitor throughout the proposed activity period, in case of fresh outbursts. However, the 2010 return was disappointing. ZHRs of ∼ 20—50 were anticipated for June 23—24, but detected ZHRs then were less than 10, and not all experienced observers confirmed even these. Prior to 1998, only three more probable returns had been detected, in 1916, 1921 and 1927, and with no significant reports between 1928 and 1997, it seemed likely these meteoroids no longer encountered Earth. The dynamics of the stream were poorly understood, although recent theoretical modelling has improved our comprehension. The shower's 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 most recent perihelion passage was in 2008 September. Clearly, the 1998 and 2004 returns resulted from material shed by the comet in the past which now lies on slightly different orbits to the comet itself. Dust trails laid down at various perihelion returns during the 19th century seem to have been responsible for the last two main outbursts. No predictions for activity are in-force for 2012, but conditions for checking are very favourable from the mid-northern latitudes where the radiant is best-seen (indeed it is usefully-observable almost all night from here), with only a waning crescent Moon on June 27. The prolonged — in some places continuous — twilight will cause difficulties, however. VID has suggested some June Boötids may be visible in most years around June 20—25, but with activity largely negligible except near λ⊙ = 92° (2012 June 23), radiating from an area about ten degrees south of the visual one found in 1998 and 2004, close to α α = 216°, δ = +38°.

5.Perseids (PER)英仙座流星雨（8月12日20时到22时30分最大100颗，月光较小）

 由IMCCE提供的流星体轨道数据图2012

 由爱尔兰阿马山天文台提供的数据2012

 

 

Active: July 17 — August 24; Maximum: August 12, 12h to 14h30m UT (λ⊙ = 140.0°—140.1°), but see text; ZHR = 100; Radiant: α = 48°, δ = +58°; Radiant drift: see Table 6; V∞ = 59 km/s; r = 2.2; TFC: α = 19°, δ = +38° and α = 348°, δ = +74° before 2h local time; α = 43°, δ = +38° and α = 73°, δ = +66° after 2h local time (β > 20° N); IFC: α = 300°, δ = +40°, α = 0°, δ = +20° or α = 240°, δ = +70° (β > 20° N).

http://www.imo.net/galleries/calendar/img/PER.jpg

The Perseids produced strong activity from an unexpected primary maximum throughout the 1990s, associated with the perihelion passage of their parent comet, 109P/Swift-Tuttle, in 1992. The comet's orbital period is about 130 years. Further enhanced activity ahead of the usual maximum was last seen in 2004. Recent IMO observations (see HMO p. 145) found the timing of the mean or "traditional" broad maximum varied between λ⊙ ∼ 139.8° to 140.3°, equivalent to 2012 August 12, 07^h to 19^h30^m UT. No additional peaks are anticipated this year, but this does not guarantee what will occur!

Although the Moon is a waning crescent, three days after last quarter on August 12, it will rise from mid-northern locations around local midnight to one a.m. Its brightness and relative proximity to the Perseid radiant should be considered more of a nuisance than a deterrent, even so. Such mid-northern latitudes are the more favoured for Perseid observing, as from here, the shower's radiant is usefully observable from 22^h—23^h local time onwards, gaining altitude throughout the night. The near-nodal part of the "traditional" maximum interval would be best-viewed from eastern Asia east to far western North America (with increasing moonlight for places further east in this zone), assuming it happens as expected. All forms of observing can be carried out on the shower, though unfortunately, it cannot be usefully observed from most of the southern hemisphere.
 

6.Draconids (DRA)（天龙座流星雨，今年也有可能爆发，极大在10月8日19时15分）

   由爱尔兰阿马山天文台提供的数据2012

 

 

Active: October 6—10; Maximum: October 8, 11h15m UT (λ⊙ = 195.4°), but see text; ZHR = periodic, up to storm levels; Radiant: α = 262°, δ = +54°; Radiant drift: negligible; V∞ = 20 km/s; r = 2.6; TFC: α = 290°, δ = +65° and α = 288°, δ = +39° (β > 30° N).

http://www.imo.net/galleries/calendar/img/DRA.jpg

The Draconids are primarily a periodic shower which produced spectacular, brief, meteor storms twice last century, in 1933 and 1946, and lower rates in several other years (ZHRs ∼ 20—500+). Most detected showers were in years when the stream's parent comet, 21P/Giacobini-Zinner, returned to perihelion, as it should next in 2012 February. Its orbital period is currently about 6.6 years. The 2011 potentially strong return was still to come when this text was written, but in 2005 October, the comet's previous perihelion year, a largely unexpected outburst happened near the nodal crossing time, around λ⊙ = 195.40°—195.44°, probably due to material shed in 1946. Visual ZHRs were ∼ 35, though radar detections suggested a much higher estimated rate, closer to ∼ 150. Outlying maximum times from the recent past have spanned from λ⊙ = 195.075° (in 1998; EZHRs ∼ 700), equivalent to 2012 October 8, 03^h20^m UT, through the nodal passage time above, to λ⊙ = 195.63°—195.76° (a minor outburst in 1999, not a perihelion-return year; ZHRs ∼ 10–20), equating to 2012 October 8, 16^h50^m to 20^h00^m UT. No predictions of unusual activity are in-force this October, but observers should be alert just in case. Last quarter Moon on October 8 makes this quite a favourable year, as the Moon rises in late evening for the many northern hemisphere locations from where the Draconid radiant is circumpolar. The radiant is at its highest during the first half of the night, and Draconid meteors are exceptionally slow-moving.
 

7.Leonids (LEO)（狮子座流星雨极不稳定，今年极大值在17日17时30分极大只有15颗每小时，但有可能更大，如果你运气好，还可以看见真正的流星雨）

  由IMCCE提供的流星体轨道数据图 2012

 由爱尔兰阿马山天文台提供的数据2012

 

 

Active: November 6—30; Maximum: November 17, 09h30m UT (nodal crossing at λ⊙ = 235.27°), but see below; ZHR = 15?; Radiant: α = 152°, δ = +22°; Radiant drift: see Table 6; V∞ = 71 km/s; r = 2.5; TFC: α = 140°, δ = +35° and α = 129°, δ = +6° (β > 35° N); or α = 156°, δ = −3° and α = 129°, δ = +6° (β < 35° N). IFC: α = 120°, δ = +40° before 0h local time (β > 40° N); α = 120°, δ = +20° before 4h local time and α = 160°, δ = 0° after 4h local time (β > 0° N); α = 120°, δ = +10° before 0h local time and α = 160°, δ = −10° (β < 0° N).

http://www.imo.net/galleries/calendar/img/LEO.jpg

The most recent perihelion passage of the Leonids' parent comet, 55P/Tempel-Tuttle, in 1998 may be nearly 15 years ago now, but the shower's activity has continued to be fascinatingly variable from year to year recently. This year seems unlikely to produce enhanced rates, but there may be more than one peak. Apart from the nodal timing above, Mikhail Maslov has suggested that there could be a peak with ZHRs of ∼ 5—10 at 21^h UT on November 17, followed by another increase to ZHRs of ∼ 10—15, probably of below-average brightness meteors, on November 20, at ∼ 06^h UT (the latter due to the 1400 AD dust-trail).

ZHRs for the nodal peak are liable to be "normal", so probably about 15±5. November's waxing Moon is excellent news for either date, as it will set before or soon after the time the Leonid radiant first becomes usefully-observable, by local midnight or so north of the equator, afterwards for places further south. All observing methods can be employed. While these potential maximum timings do not exclude all others, if they prove correct, the two November 17 ones would be best-detectable from North American, and Middle East to Asian longitudes respectively, while that on November 20 would be similarly available from places between eastern North America east to extreme western North African longitudes.

8.α-Monocerotids (AMO)麒麟座α流星雨（11月21日17时55分极大，极大值一般到5颗，今年可能爆发到400颗每小时）

 

 

 

Active: November 15—25; Maximum: November 21, 09h55m UT (λ⊙ = 239.32°); ZHR = variable, usually ∼ 5, but may produce outbursts to ∼ 400+; Radiant: α = 117°, δ = +1°; Radiant drift: see Table 6; V∞ = 65 km/s; r = 2.4; TFC: α = 115°, δ = +23° and α = 129°, δ = +20° (β > 20° N); or α = 110°, δ = −27° and α = 98°, δ = +6° (β < 20° N).

http://www.imo.net/galleries/calendar/img/AMO.jpg

The α–Monocerotids gave their most recent brief outburst in 1995 for Europe (the top EZHR, ∼ 420, lasted five minutes, the entire outburst 30 minutes). Recent modelling by Esko Lyytinen has indicated the main AMO trail will not cross the Earth's orbit again until 2017 and 2020. However, the Earth will not be near those points in November, so nothing is likely to happen then. A weak return may occur in November 2019, ahead of the 2020 encounter, depending on how broad the trail may be. The next strong AMO outburst is unlikely before 2043.

Despite this, observers should monitor the AMO closely in every year possible, in case of unanticipated events. The brevity of all past outbursts means breaks under clear skies should be kept to a minimum near the predicted peak. The waxing gibbous Moon causes few problems for the maximum date this year, as the shower's radiant is well on view from either hemisphere after about 23^h local time, with moonset around 00^h—01^h (later further north). If correct, the peak timing would fall well for sites across North America.
 

9.Phoenicids (PHO)12月6日11时45分凤凰座流星雨极大，通常几乎没有，但是也有可能爆发到100，那就要看运气了

 由IMCCE提供的流星体轨道数据图 2012

 

 

Active: November 28 — December 9; Maximum: December 6, 03h45m UT (λ⊙ = 254.25°); ZHR = variable, usually none, but may reach 100; Radiant: α = 18°, δ = −53°; Radiant drift: see Table 6; V∞ = 18 km/s; r = 2.8; TFC: α = 040°, δ = −39° and α = 065°, δ = −62° (β < 10° N).

http://www.imo.net/galleries/calendar/img/PHO.jpg

Only one impressive Phoenicid return has been reported so far, that of its discovery in 1956, when the EZHR was probably ∼ 100, possibly with several peaks spread over a few hours. Three other potential, if uncertain, bursts of lower activity have been claimed. Reliable IMO data has shown recent activity to have been virtually nonexistent. This may be a periodic shower however, and more observations of it are needed by all methods. From the southern hemisphere (only), the Phoenicid radiant culminates at dusk, remaining well on view for most of the night. Last quarter Moon rises soon after midnight, leaving the first half of the night with dark skies for observers on December 6. As the predicted possible 2011 return was still to come when this was written, any activity then may help refine the shower’s parameters given here. No predictions of activity are in-force for 2012. Phoenicids are extremely slow meteors.
 

10.Geminids (GEM)（双子座流星雨，每年最值得看的最稳定的流星雨，昨年受月光影响，今年将完全不会，理论期望值每半分钟1颗流星，今年最大值在12月14日7时30分，欧洲观测最佳，中国也不错哟！）

 由IMCCE提供的流星体轨道数据图2012

 

 

 

Active: December 4—17; Maximum: December 13, 23h30m UT (λ⊙ = 262.2°); ZHR = 120; Radiant: α = 112°, δ = +33°; Radiant drift: see Table 6; V∞ = 35 km/s; r = 2.6; TFC: α = 87°, δ = +20° and α = 135°, δ = +49° before 23h local time, α = 87°, δ = +20° and α = 129°, δ = +20° after 23h local time (β > 40° N); α = 120°, δ = −3° and α = 84°, δ = +10° (β < 40° N). IFC: α = 150°, δ = +20° and α = 60°, δ = +40° (β > 20° N); α = 135°, δ = -5° and α = 80°, δ = 0° (β < 20° N).

http://www.imo.net/galleries/calendar/img/GEM.jpg

One of the finest, and probably the most reliable, of the major annual showers presently observable, whose peak this year falls perfectly for new Moon. Well north of the equator, the radiant rises about sunset, reaching a usable elevation from the local evening hours onwards. In the southern hemisphere, the radiant appears only around local midnight or so. It culminates near 02^h. Even from more southerly sites, this is a splendid stream of often bright, medium-speed meteors, a rewarding event for all observers, whatever method they employ. The peak has shown slight signs of variability in its rates and timing in recent years, with the more reliably-reported maxima during the past two decades (HMO, p. 171) all having occurred within λ⊙ = 261.5° to 262.4°, 2012 December 13, 07^h to December 14, 04^h UT. Near-peak rates usually persist for almost a day, so much of the world has the chance to enjoy something of the Geminids’ best. Some mass-sorting within the stream means fainter telescopic meteors should be most abundant almost a day ahead of the visual maximum, with telescopic results indicating such meteors radiate from an elongated region, perhaps with three sub-centres. Further results on this topic would be useful.
 

11.Ursids (URS)（小熊座流星雨，每年最后出场的算比较大的流星雨，今年极大值在12月22日16时极大值只有10颗每小时，偶尔也可能会有50颗，又要靠运气行事了）

 由IMCCE提供的流星体轨道数据图  2012

 

 

 

Active: December 17—26; Maximum: December 22, 08h UT (λ⊙ = 270.7°), but see below; ZHR = 10 (occasionally variable up to 50); Radiant: α = 217°, δ = +76°; Radiant drift: see Table 6; V∞ = 33 km/s; r = 3.0; TFC: α = 348°, δ = +75° and α = 131°, δ = +66° (β > 40° N); α = 063°, δ = +84° and α = 156°, δ = +64° (β 30° to 40° N).

http://www.imo.net/galleries/calendar/2011/urs.png

A very 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 have been reported as well, most recently from 2006–2008 inclusive which were probably influenced by the relative proximity of the shower's parent comet, 8P/Tuttle, at perihelion in January 2008. Other events could have been easily missed. Jérémie Vaubaillon suggests there could be another peak this year, around 03^h01^m UT on December 22, with ZHRs of ∼ 15. The Ursid radiant is circumpolar from most northern sites (thus fails to rise for most southern ones), though it culminates after daybreak, and is highest in the sky later in the night. The waxing gibbous Moon at the maximum will set by roughly two a.m. from mid northern sites, so this return is not unfavourable. The ∼ 03^h timing would be best-seen from European longitudes with no Moon, while the ∼ 08^h peak would be good for eastern North America similarly

更多流星雨2012
想要了解更多可以查由法国计算的流星雨体轨道图http://tianxiangyubao.happymm.cn/script/forum/view.asp?article_id=783435

以及爱尔兰阿马山天文台提供的数据图http://tianxiangyubao.happymm.cn/script/forum/view.asp?article_id=785737

有关2012年流星雨的更多信息：

1. 2012年主要大流星雨（主要来自IMO）

2. 2012年主要流星雨时间表（IMO）

3. 2012年主要大流星雨（表）

4. 2012年南半球主要流星雨（由新西兰皇家天文学会提供）仅作参考

5. 2012年流星雨（由法国提供的流星体轨道图）

6. 2012年主要流星雨月相参考

7. 2012年流星雨撮要（香港天文学会）

8. 2012年流星雨月相撮要 （香港天文学会）

9. 1月  2月   3月  4月  5月  6月  7月   8月  9月  10月  11月  12月

10.2012年12月14日双子座流星雨