The Taurid meteor complex daytime streams Zeta Perseids and Beta Taurids are investigated from the viewpoint of their orbital evolution and relation to the streams of the preperihelion branch of the complex. A search for potential

co-parents among NEOs known until mid-June 2005 is made and two candidates for the association with the Zeta Perseids and two for the Beta Taurids are found. The Beta Taurids are shown to be postperihelion continuation of the Northern Taurids and Zeta Perseids are continuation of two complex filaments related to the Southern Taurids

Cevolani, G.

Kornoš, L.

Pecina, P.

Porubčan, V.

Pupillo, G.

English

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NOTE BREVIDOI 10.1393/ncc/i2005-10203-5IL NUOVO CIMENTO Vol. 28 C, N. 6 Novembre-Dicembre 2005On the association of the daytime Taurid complex meteor streamswith asteroidsV. Porubcˇan(1), L. Kornosˇ(1), P. Pecina(2), G. Cevolani(3)and G. Pupillo(3)(4)(1) Department of Astronomy, Physics of the Earth and MeteorologyFMPI Comenius University - 842 48 Bratislava, Slovakia(2) Astronomical Institute of the Academy of Sciences of the Czech Republic251 65 Ondrˇejov, Czech Republic(3) CNR-ISAC - via Gobetti 101, 40129 Bologna, Italy(4) Osservatorio di Campi Salentina - 73012 Campi Salentina (Lecce), Italy(ricevuto l’11 Novembre 2005; approvato il 29 Dicembre 2005; pubblicato onlineil 18 Gennaio 2006)Summary. — The Taurid meteor complex daytime streams Zeta Perseids and BetaTaurids are investigated from the viewpoint of their orbital evolution and relationto the streams of the preperihelion branch of the complex. A search for potentialco-parents among NEOs known until mid-June 2005 is made and two candidates forthe association with the Zeta Perseids and two for the Beta Taurids are found. TheBeta Taurids are shown to be postperihelion continuation of the Northern Tauridsand Zeta Perseids are continuation of two complex filaments related to the SouthernTaurids.PACS 96.50.Kr – Meteors and meteoroids.PACS 95.85.Bh – Asteroids.1. – IntroductionWhipple already in 1940 in his analysis of photographic meteor orbits of the Tauridstream [1] suggested that due to a low inclination the stream has to cross the Earth’sorbit also in its postperihelion passage in June-July and could be observed as a daytimestream. The stream was first detected at the Jodrell Bank Observatory in 1947 [2] by theobservatory radio equipment as the Zeta Perseids active in June 2-17 and Beta Tauridsactive in June 20-27. The radio observations in the following years carried out at JodrellBank and other observatories revealed longer activity periods of the streams in the periodMay-July and enabled to determine also the orbits of individual meteors, e.g. [3-7].There were practicaly no studies of the activity of the streams after 1960’s. The mostcurrent investigation of the activity and mass distribution based on forward scatter ob-servations by the BLM equipment (Budrio-Lecce-Modra, Italy-Slovakia) and backscatterradio observations by the Ondrˇejov meteor radar (Czech Republik) was performed byPupillo et al. [8] and Pecina et al. [9].c© Societa` Italiana di Fisica 933934 V. PORUBCˇAN, L. KORNOSˇ, P. PECINA ETC.Table I. – The mean orbits of the Zeta Perseids and Beta Taurids derived from radio observa-tions (postperihelion), the associated Taurid filaments derived from photographic data (preperi-helion) and NEOs potentially related to them.Stream q (AU) a (AU) e i (◦) ω(◦) Ω(◦) π(◦) NumberZeta PerseidsCook [13] 0.34 1.6 0.79 0.0 59.0 78.7 137.7Sekanina [6] 0.319 1.918 0.834 5.3 59.2 78.3 137.5 73Beta TauridsCook [13] 0.34 2.2 0.85 6.0 246.0 277.1 163.1Sekanina [6] 0.325 1.853 0.825 2.2 239.2 275.2 154.4 57Taurid filaments [10]Tau 04 0.338 1.465 0.770 6.1 121.8 359.5 121.3 5Tau 05 0.318 1.925 0.837 5.7 120.1 10.9 131.0 5Southern Taurids 0.365 2.187 0.833 5.3 113.1 43.3 156.4 56Northern Taurids 0.358 2.174 0.835 2.7 293.7 228.6 162.3 381999 RK45 0.363 1.598 0.773 5.9 4.0 120.1 124.12003 QC10 0.369 1.377 0.732 5.0 120.4 0.3 120.72003 UV11 0.344 1.451 0.763 5.9 124.6 32.2 156.82004 TG10 0.315 2.242 0.860 3.7 310.0 212.3 162.3In the present paper a possible association of the near-Earth’s objects (NEOs) movingclose to the Taurid meteor complex daytime streams the Zeta Perseids and Beta Taurids isinvestigated. The study is based on following the orbital similarity and orbital evolutionof both streams and NEOs potentially associated with them.2. – AnalysisPorubcˇan et al. [10] have recently investigated the structure of the Taurid meteorcomplex (TMC) and searched for potential co-parents of the complex or its streams andfilaments among all NEOs known until the mid-June 2005 (3380 objects in the AsteroidOrbital Elements Database managed by T. Bowell, Lowell Observatory). In the firststep a stream search utilizing the Southworth-Hawkins D criterion [11] was applied tothe sample of photographic meteor orbits of the Meteor Data Center catalogue [12]. Toget the cores or central parts of the streams or sub-streams a strict limiting value ofD ≤ 0.1 was applied and up to twenty filaments relating to the Taurid complex could beselected.Further a search for NEOs to be potentially associated with the Taurid filaments wasmade. In the first step orbital similarity was verified by comparing the mean orbits ofthe filaments with the orbits of NEOs applying the D criterion which for two orbits inspace defines a distance function in terms of the osculating orbital elements (q, e, i, ω,Ω). 91 asteroids were found moving close to the complex within the value of D ≤ 0.3. Inthe next step their potential association with the filaments was verified by following theorbital evolution of both the asteroids and filaments. As a result, possible associationsbetween 8 TMC filaments and 15 NEOs were revealed.ON THE ASSOCIATION OF THE DAYTIME TAURID COMPLEX METEOR STREAMS ETC. 935Fig. 1. – Backward integration of the orbits of the Zeta Perseids and asteroids 1999 RK45 and2003 QC10 over 5000 years and related Southworth-Hawkins D criterion value.For the present analysis, we have applied the same procedure in order to look forasteroids moving close to the streams of the Taurid meteor complex in its postperihelionpassage observed as the daytime streams Zeta Perseids and Beta Taurids. Both streamsare members of a huge complex of different sub-streams belonging to the TMC and onecan expect that the same bodies or at least the majority of them will be close to bothpreperihelion and postperihelion branches of the TMC.The orbital elements of the Zeta Perseids and Beta Taurids can be obtained fromradio observations only and the most compact information so far, including all basicparameters, the activity periods, radiants, velocities and mean orbits were published by936 V. PORUBCˇAN, L. KORNOSˇ, P. PECINA ETC.Fig. 2. – Backward integration of the orbits of the Beta Taurids, asteroids 2003 UV11 and 2004TG10 over 5000 years and related Southworth-Hawkins D criterion value.Cook [13] and Sekanina [6, 7]. The corresponding mean orbits for both the streams arelisted in table I. The mean orbits by Sekanina are based on 73, respectively 57, individualorbits and were obtained in the frame of the Harvard Radio Meteor Project in 1960th.The angular elements in table I are referred to equinox 2000.0.In the first step of the analysis the NEOs moving close to the streams were searchedfor by comparison of the osculating orbits of known NEOs (3380 objects known until mid-June 2005) with the mean orbits of the Zeta Perseids and Beta Taurids listed in table I.Due to the fact that the mean orbits published by Sekanina [6] are based on relativelylarge sets of individual orbits and were obtained by the same equipment (Cook does notON THE ASSOCIATION OF THE DAYTIME TAURID COMPLEX METEOR STREAMS ETC. 937Table II. – Basic parameters of the Taurid meteor complex postperihelion streams and potentiallyassociated asteroids.Stream R.A. Dec. Vg H Diameter DSH Period(◦) (◦) (km/s) (mag.) (m) (y)Zeta Perseids [6] 60 25 291999 RK45 47 21 24 19.32 360 0.12-0.20 17002003 QC10 43 19 24 17.83 800 0.18-0.20 1000Beta Taurids [6] 80 22 282003 UV11 83 25 26 19.30 410 0.20-0.15 20002004 TG10 88 23 30 19.40 390 0.20-0.08 2500list from how large sets are the mean orbits of the streams derived, neither sources), theHarvard orbits were chosen as the reference mean orbits for the Zeta Perseids and BetaTaurids. For the analysis only asteroids for which the value of D ≤ 0.3 were selected andthus 19 NEAs were found moving close to the both daytime streams.The orbital similarity of two osculating orbits cannot be conclusive for a decisionabout an association between bodies moving in them. More conclusive is a study ofthe orbital evolution. Followingly, to study the associations between the Zeta Perseids,the Beta Taurids and asteroids the orbital evolution of the mean orbits of the streamsand all 19 asteroids was investigated. We have applied for the backward integration ofthe orbital evolution the multistep procedure of Adams-Bashforth-Moulton’s type up to12th order, with variable step-size, developed by Shampine and Gordon [14]. Thoughmeteoroid streams can be typically recognized over a time scale 103–104 years, we havefollowed the orbital evolution of all the bodies for 5000 years, the time which could beconsidered sufficient to indicate on potential associations between the studied objects.In the next step only asteroids for which the value of D over the period of integrationwas D ≤ 0.20, were considered for relatively close to the streams and as possible candi-dates for co-parents. In this way asteroids 1999 RK45, 2003 QC10 can be associated tothe Zeta Perseids and asteroids 2003 UV11 and 2004 TG10 to the Beta Taurids.The results of integration are presented on plots in fig. 1 and fig. 2. In the plots, thereare diagrams depicting the evolution of the orbital elements: perihelion distance (q),eccentricity (e), inclination (i), argument of perihelion (ω) and longitude of perihelion(π) over 5000 years. Figures 1 and 2 also show the variation of the D criterion describingthe degree of similarity between the orbits of the Zeta Perseids, the Beta Taurids andcorresponding asteroids, respectively.All the four asteroids are moving close also to the autumn Taurid stream [10] andare probable co-parents of the N and S Taurids (2003 UV11, 2004 TG10) and of twofilaments Tau 05 and Tau 07 from the beginning of the Taurid complex activity relatedto the S Taurids (1999 RK45 and 2003 QC10). The mean orbits of the filaments as wellas of the associated asteroids are listed in table I.Basic information on “possible” associations between the Zeta Perseids, the BetaTaurids and NEOs are summarized in table II, where besides the theoretical meteorradiants [15] and geocentric velocity are listed also the absolute magnitude of the asteroidH, the diameter in meters defined from the albedo A = 0.05, the change of D criterionvalue and period of integration in which D ≤ 0.20.Comparison of the orbital evolution of the Zeta Perseids and Beta Taurids with the938 V. PORUBCˇAN, L. KORNOSˇ, P. PECINA ETC.probable associated asteroids over the period of integration of 5000 years (figs. 1, 2)assessed by the Southworth-Hawkins criterion DSH indicates a close association betweenthe Beta Taurids and asteroids 2003 UV11 and 2004 TG10 over the last 2000–2500 years.The radiant position and geocentric velocity in table II refer to the osculating orbits. Onthe association of the Zeta Perseids with asteroids 1999 RK45, 2003 QC10 can be inferredfor about 5000-3000 years ago when the asteroids were very close to the stream and couldtake part in the stream generation.3. – ConclusionsThe spring/summer Taurid complex meteoroid streams, the Zeta Perseids and BetaTaurids with the peak activity about June 9 and June 29, respectively, were searched forpotential co-parents. Of the 3380 NEOs known until the mid-June 2005, 19 objects werefound to move close to the streams satisfying the Southworth-Hawkins criterion valueD ≤ 0.30.Following the orbital evolution of the streams and NEOs over 5000 years, four aster-oids over the period of integration kept the value of D ≤ 0.20 and can be considered forrelated to the streams: 1999 RK45, 2003 QC10 to the Zeta Perseids and 2003 UV11,2004 TG10 to the Beta Taurids. All four asteroids are moving also close to the autumnTaurids and are probable co-parents of their northern and southern branches.The Beta Taurids are postperihelion continuation of the Northern Taurids. The ZetaPerseids are continuation of the Southern Taurids and of two filaments from the ascendingbranch of the TMC activity related to the Southern Taurids.The asteroids moving within the Zeta Perseids and Beta Taurids are small bodies, insize smaller than one kilometer and taking into account present systematic monitoring ofthe sky, it can be expected that new additional NEOs of sizes up to few hundred metersmoving in the Taurid meteor complex will be discovered soon.∗ ∗ ∗The authors are indebted for the support of the research to VEGA, the Slovak GrantAgency for Science, grant No. 1/0204/03 and to the Grant Agency of Czech Republic,grant No. 205/03/1405.REFERENCES[1] Whipple F. L., Proc. Am. Philos. Soc., 83 (1940) 711.[2] Kronk G. W., Meteor Showers: A Descriptive Catalogue (Enslow Publ., Hillside, USA)1988.[3] Aspinall A. and Hawkins G. S., Mon. Not. R. Astron. Soc., 111 (1951) 18.[4] Kashcheyev B. L. and Lebedinets V. N., Smithson. Contrib. Astrophys., 11 (1967)183.[5] Gartrell G. and Elford W. G., Aust. J. Phys., 28 (1975) 591.[6] Sekanina Z., Icarus, 18 (1973) 253.[7] Sekanina Z., Icarus, 27 (1976) 265[8] Pupillo G., Porubcˇan V., Pecina P., Pecinova´ D., Cevolani G. and Zigo P., NuovoCimento C, 28 (2006) submitted.[9] Pecina P., Porubcˇan V., Pecinova´ D. and To´th J., Earth, Moon and Planets, 95(2005) in print.[10] Porubcˇan V., Kornosˇ L. and Williams I. P., Contrib. Astron. Obs. Skalnate Pleso, 36(2006) submitted.ON THE ASSOCIATION OF THE DAYTIME TAURID COMPLEX METEOR STREAMS ETC. 939[11] Southworth R. B. and Hawkins G. S., Smithson. Contrib. Astrophys., 7 (1963) 261.[12] Lindblad B. A., Neslusˇan L., Porubcˇan V. and Svorenˇ J., Earth, Moon, and Planets,93 (2003) 249.[13] Cook A. F., Evolutionary and Physical Properties of Meteoroids, edited by HemenwayC. L., Millman P. M. and Cook A. F. (1973), p. 183.[14] Shampine L. F. and Gordon M. K., Computer Solution of Ordinary DifferentialEquations (Freeman and Comp., San Francisco) 1975.[15] Neslusˇan L., Svorenˇ J. and Porubcˇan V., Astron. Astrophys., 331 (1998) 411.

On the association of the daytime Taurid complex meteor streams with asteroids

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On the association of the daytime Taurid complex meteor streams with asteroids

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