- Email: [email protected]
Don Quixote—A possible parent body of a meteor shower
Planetary and Space Science ∎ (∎∎∎∎) ∎∎∎–∎∎∎
Contents lists available at ScienceDirect
Planetary and Space Science journal homepage: www.elsevier.com/locate/pss
Don Quixote—A possible parent body of a meteor shower Regina Rudawska a,n, Jeremie Vaubaillon b a b
Comenius University, Faculty of Mathematics, Physics and Informatics, Mlynská dolina, Bratislava SK-84248, Slovakia Institut de Mécanique Céleste et de Calcul des Éphémérides - Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris, France
art ic l e i nf o
a b s t r a c t
Article history: Received 22 January 2015 Received in revised form 13 April 2015 Accepted 22 April 2015
Asteroid 3552 Don Quixote (1983 SA) orbits the Sun on an orbit that resembles that of a short-period comet. This, together with its recently observed cometary activity, makes it a good candidate for a parent body of a meteor shower. Model calculations show that the particles originated from Don Quixote pass close enough to Earth orbit to search for a meteor shower activity. Corresponding meteor showers were found in CAMS (Rudawska and Jenniskens, 2014) and EDMOND (Kornoš et al., 2014) video observations. The κ Lyrids and August μ Draconids (IAU#464 and IAU#470, respectively), a similarly inclined stream active in the summer, are associated with 3552 Don Quixote. & 2015 Elsevier Ltd. All rights reserved.
Keywords: Meteor shower Meteoroid stream Comet Asteroid
1. Introduction Meteoroid streams originate during processes that occur on a surface of a comet (when it approaches the Sun) or on a surface of an asteroid (e.g. when asteroids collide). After abandoning the parent body, meteoroids start their journey in space, occupying similar orbits that creates a structure called meteoroid stream. When particles of the stream enter the Earth's atmosphere, they create phenomena called meteor shower. A given parent body can give origin to more than one meteor shower; e.g. 1P/Halley is a parent body of the Orionids and η Aquarids (Babadzhanov et al., 2008; Wiegert and Brown, 2004; Brown et al., 2008, 2010, Neslušan et al., 2014a,b, Rudawska et al., 2012; Rudawska and Jenniskens, 2014). Parent bodies also create dynamical groups (Asher et al., 1993; Babadzhanov, 2001), and give origin to complex meteoroid streams (e.g. Taurids complex. There are also NEAs thought to be extinct cometary nuclei, but which start to show cometary activity (Jewitt, 2012). Automated surveys of Near-Earth Objects (NEOs) continue to discover objects in cometary-like orbits that are likely candidate parent bodies. These have orbits with Tisserand parameters between 2 and 3, typical of Jupiter Family Comets. Some of those come close to Earth orbit, but are not associated with meteor shower activity. Here, we study the case of asteroid 3552 Don Quixote (1983 SA). At first there was no activity observed from Don Quixote when it n
Corresponding author. E-mail address: [email protected] (R. Rudawska).
approached the Sun. This was till recently when a tail was spotted from Don Quixote (Mommert et al., 2014). Asteroid (3552) Don Quixote was discovered in 1983 and categorized as Amor asteroid. It is an object of about 12.3–24.5 km diameter, low-albedo, spectral type D, and orbit which resembles that of a comet (the Tisserand parameter for the orbit has a value of 2.315 with respect to Jupiter). This observed activity makes Don Quixote a good candidate for a short-period comet among known NEOs. The question arises of whether a meteor shower can be created from Don Quixote? If so, do/did we observe it on Earth? In Section 2 we describe the method we applied. Section 3 focuses on the results, while Section 4 presents our conclusions.
2. Methodology In order to answer questions that arose in Section 1 our methodology combines two steps: meteoroid stream modelling, and search for similarity between the orbits of simulated stream and orbits of known meteoroid streams. Table 1 Orbital elements of 3552 Don Quixote (1983 SA). Source: JPL HORIZONS website.
q (AU)
e
i (deg)
ω (deg)
Ω (deg)
1.2099
0.71324
30.98
317.03
350.27
http://dx.doi.org/10.1016/j.pss.2015.04.014 0032-0633/& 2015 Elsevier Ltd. All rights reserved.
Please cite this article as: Rudawska, R., Vaubaillon, J., Don Quixote—A possible parent body of a meteor shower. Planetary and Space Science (2015), http://dx.doi.org/10.1016/j.pss.2015.04.014i
R. Rudawska, J. Vaubaillon / Planetary and Space Science ∎ (∎∎∎∎) ∎∎∎–∎∎∎
2
Table 2 Geocentric and orbital parameters of κ Lyrids and August μ Draconids. Source: IAU MDC. Stream
λ⊙ (deg)
α (deg)
δ (deg)
Vg (km/s)
q (AU)
e
ω (deg)
Ω (deg)
i (deg)
#464 KLY #470 AMD
126.9 145.4
277.5 253.7
þ 33.3 þ 58.8
18.6 19.5
0.939 1.011
0.698 0.654
215.1 177.2
126.8 145.4
24.7 30.3
3. Results
Table 3 Mean orbital elements of simulated meteoroid stream.
3.1. Possibly associated meteor showers q (AU)
e
ω (deg)
Ω (deg)
i (deg)
0.981
0.680
197.4
144.1
28.3
2.1. Meteoroid stream modelling We have investigated the orbital evolution of the meteoroid stream originating from Don Quixote asteroid. For this purpose we modelled the meteoroid stream originated from Don Quixote and its evolution in the Solar System. The model of generation and evolution of meteoroid stream in the solar system is taken from Vaubaillon et al. (2005). The initial orbital elements and physical properties of the object are taken from JPL HORIZONS website1 (Table 1), and integrated over an arc of orbit within three astronomical units. Each time the object approached the Sun, meteoroids were released at regular time intervals (one day) within 3 AU from the Sun. Ejection in a hemisphere towards the Sun is assumed with mass-dependent velocities taken from Crifo and Rodionov (1997). The ejections of 5000 meteoroids from the object's surface took place every 100 years when it was passing its perihelion between 5000 B.C. and 2013 A.D. Next, the orbits of the ejected meteoroids were integrated to year 2050 A.D. For this purpose, we used a 15th order Radau integrator (Everhart, 1985), while meteoroid orbits were controlled by gravitational and nongravitational forces (radiation pressure, Poynting–Robertson drag, and Yarkovky's effect). If a meteoroid is sufficiently close to the Earth, its orbital parameters are saved and compared with known showers. The theoretical radiant of a meteoroid orbit that passed within 0.05 AU from Earth is calculated with the Q method (Hasegawa, 1990) using Neslusan et al. (1998) software, which adjusts for the miss-distance by changing the perihelion distance. 2.2. Similarity functions The similarity between the orbits of the particles reaching the Earth with orbits of known meteoroid streams listed at the International Astronomical Union Meteor Data Center (IAU MDC) needs to be quantified. Many tests have been proposed to measure the difference between orbits and have recently been discussed in Jopek and Williams (2013). The most popular is that of Southworth and Hawkins (1963), but we choose to use the newer and more robust criterion of Jopek et al. (2008) described by heliocentric vectorial elements, namely
DV2 = wh1 (hB1 − hA1 )2 + wh2 (hB2 − hA2 )2 + 1.5 wh3 (hB3 − hA3 )2 + we1 (eB1 − eA1 )2 + we2 (eB2 − eA2 )2 + we3 (eB3 − eA3 )2 + 2wE (EB + EA )2 ,
(1)
where h A and h B are the angular momenta, e A and eB are the Laplace vectors, EA and EB are the orbital energy of two orbits, and w are weight coefficients. In the survey, we used values of weight coefficients taken from Jopek et al. (2008). 1
http://ssd.jpl.nasa.gov/?horizons
Using the method described in the previous section we found two meteor showers: κ Lyrids (#464, KLY), and August μ Draconids (#470, AMD). Both meteor showers remain on the working list of the IAU MDC2 (Table 2). κ Lyrids and August μ Draconids meteor showers were first identified in a cluster analysis applied to the combined meteoroid orbit database derived from low-light level video observations by the SonotaCo consortium in Japan (SonotaCo, 2009) and by the Cameras for All-sky Meteor Surveillance (CAMS; Jenniskens et al., 2011) project in California, USA (Rudawska and Jenniskens (2014). AMD shower consisted 6 orbits, where 5 of them were meteors detected by CAMS. In case of KLY meteor shower, 5 out of 6 meteors were observed by SonotaCo. Kornoš et al. (2014), using the radiant position-geocentric velocity method, also identified those showers in the 4th version of the EDMOND database (Kornos et al., 2013). We compare the orbits of κ Lyrids and August μ Draconids (Table 2) with orbits from our simulation (Table 3), using DV, we achieved a good match. The obtained values of DV for KLY and AMD meteor showers (0.05 and 0.05, respectively) are below conventional threshold value assumed when establishing orbits similarity, i.e. 0.08 (Jopek et al., 2008; Rudawska et al., 2012). 3.2. Radiants' distribution In Fig. 1, we compare all modelled meteors with observed κ Lyrids and August μ Draconids meteor showers. The theoretical radiant of a meteoroid orbit that passed sufficiently close to Earth is calculated with the Q method (Hasegawa, 1990). The distribution of theoretical radiant plotted together with radiant position of KLY and AMD taken from the IAU MDC as well as with KLY and AMD identified by independent identification method applied to the latest version of the EDMOND database (Rudawska et al., 2014). The position of both showers taken from the IAU MDC nicely fits the simulated meteor shower, occupying two parts of the simulated shower. Moreover, when we add members of both meteor showers found in the EDMOND database by the independent method, we notice that the observed dispersion of radiants is in excellent agreement with the simulated distribution.
4. Conclusion This paper addresses the topic of the meteoroid stream of a parent body in relation to meteor showers observed on Earth. We carried out a search to investigate the possibility of meteor shower observations caused by particles ejected from 3552 Don Quixote (1983 SA). We showed that if Don Quixote did eject a meteoroid stream in the past 5000 years, it would produce meteor showers on Earth today that match the observed κ Lyrids and μ Draconids. This is a 2
http://www.astro.amu.edu.pl/ jopek/MDC2007/
Please cite this article as: Rudawska, R., Vaubaillon, J., Don Quixote—A possible parent body of a meteor shower. Planetary and Space Science (2015), http://dx.doi.org/10.1016/j.pss.2015.04.014i
R. Rudawska, J. Vaubaillon / Planetary and Space Science ∎ (∎∎∎∎) ∎∎∎–∎∎∎
Fig. 1. Radiant position for simulated meteor shower ( ), κ Lyrids ( ) and August μ Draconids ( ) taken from IAU MDC (Table 2), and κ Lyrids ( ) and August μ Draconids ( ) identified in EDMOND database by Rudawska et al. (2014).
necessary step towards the association between these showers and Don Quixote. A total of 11 orbits of κ Lyrids and August μ Draconids from IAU MDC were taken into account in this study. Future additional orbital data would be extremely useful to definitely prove without ambiguity the parenthood of Don Quixote with these two showers.
References Asher, D.J., Clube, S.V.M., Steel, D.I., 1993. Asteroids in the Taurid complex. Mon. Not. R. Astron. Soc. 264 (September), 93. Babadzhanov, P.B., 2001. Search for meteor showers associated with Near-Earth Asteroids. I. Taurid Complex. Astron. Astrophys. 373 (July), 329–335. http://dx. doi.org/10.1051/0004-6361:20010583. Babadzhanov, P.B., Williams, I.P., Kokhirova, G.I., 2008. Meteor showers associated with 2003EH1. Mon. Not. R. Astron. Soc. 386 (June), 2271–2277. http://dx.doi. org/10.1111/j.1365-2966.2008.13202.x. Brown, P., Weryk, R.J., Wong, D.K., Jones, J., 2008. A meteoroid stream survey using the Canadian Meteor Orbit Radar. I. Methodology and radiant catalogue. Icarus 195 (May), 317–339. http://dx.doi.org/10.1016/j.icarus.2007.12.002. Brown, P., Wong, D.K., Weryk, R.J., Wiegert, P., 2010. A meteoroid stream survey using the Canadian Meteor Orbit Radar. II: Identification of minor showers using a 3D wavelet transform. Icarus 207 (May), 66–81. http://dx.doi.org/ 10.1016/j.icarus.2009.11.015.
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Crifo, J.F., Rodionov, A.V., 1997. The dependence of the circumnuclear coma structure on the properties of the nucleus. Icarus 127 (June), 319–353. http://dx.doi. org/10.1006/icar.1997.5690. Everhart, E., 1985. An efficient integrator that uses Gauss–Radau spacings. In: Carusi, A., Valsecchi, G.B. (Eds.), Dynamics of Comets: Their Origin and Evolution, Proceedings of IAU Colloq. 83, held in Rome, Italy, June 11–15, 1984, Astrophysics and Space Science Library, vol. 115. Riedel, Dordrecht, 1985, p. 185. Hasegawa, I., 1990. Predictions of the meteor radiant point associated with a comet. Astron. Soc. Jpn. 42 (February), 175–186. Jenniskens, P., Gural, P.S., Dynneson, L., Grigsby, B.J., Newman, K.E., Borden, M., Koop, M., Holman, D., 2011. CAMS: Cameras for Allsky Meteor Surveillance to establish minor meteor showers. Icarus 216 (November), 40–61. http://dx.doi. org/10.1016/j.icarus.2011.08.012. Jewitt, D., 2012. The active asteroids. Astron. J. 143 (March), 66. http://dx.doi.org/ 10.1088/0004-6256/143/3/66. Jopek, T.J., Rudawska, R., Bartczak, P., 2008. Meteoroid stream searching: the use of the vectorial elements. Earth Moon Planets 102 (June), 73–78. http://dx.doi.org/ 10.1007/s11038-007-9197-8. Jopek, T.J., Williams, I.P., 2013. Stream and sporadic meteoroids associated with near-Earth objects. Mon. Not. R. Astron. Soc. 430 (April), 2377–2389. http://dx. doi.org/10.1093/mnras/stt057. Kornos, L., Koukal, J., Piffl, R., Toth, J., 2013. Database of meteoroid orbits from several European video networks. In: Gyssens, M., Roggemans, P. (Eds.), Proceedings of the International Meteor Conference, 31st IMC, La Palma, Canary Islands, Spain, 2012, January, pp. 21–25. Kornoš, L., Matlovič, P., Rudawska, R., Tóth, J., Hajduková, M., Koukal, J., Piffl, R., 2014. Confirmation and characterization of IAU temporary meteor showers in EDMOND database. ArXiv e-prints, May. Mommert, M., Hora, J.L., Harris, A.W., Reach, W.T., Emery, J.P., Thomas, C.A., Mueller, M., Cruikshank, D.P., Trilling, D.E., Delbo, M., Smith, H.A., 2014. The discovery of cometary activity in near-earth asteroid (3552) Don Quixote. Astrophys. J. 781 (January), 25. http://dx.doi.org/10.1088/0004-637X/781/1/25. Neslusan, L., Svoren, J., Porubcan, V., 1998. A computer program for calculation of a theoretical meteor-stream radiant. Astron. Astrophys. 331 (March), 411–413. Neslušan, L., Hajduková, M., Tomko, D., Kaňuchová, Z., Jakubík, M., 2014a. The prediction of meteor showers from all potential parent comets. In: Rault, J.-L., Roggemans, P. (Eds.), Proceedings of the International Meteor Conference, Giron, France, 18–21 September 2014, February, pp. 139–145. Neslušan, L., Kaňuchová, Z., Tomko, D., 2014b. The ecliptic-toroidal structure of the meteor complex of comet 96P/Machholz. Meteoroids 2013 (July), 235–242. Rudawska, R., Jenniskens, P., 2014. New meteor showers identified in the CAMS and SonotaCo meteoroid orbit surveys. Meteoroids 2013 (July), 217–224. Rudawska, R., Matlovič, P., Tóth, J., Kornoš, L., 2014. Independent identification of meteor showers in EDMOND database. In: Rault, J.-L., Roggemans, P. (Eds.), Proceedings of the International Meteor Conference, Giron, France, 18–21 September 2014, February, pp. 98–100. Rudawska, R., Vaubaillon, J., Atreya, P., 2012. Association of individual meteors with their parent bodies. Astron. Astrophys. 541 (May), A2. http://dx.doi.org/10.1051/ 0004-6361/201118762. SonotaCo, 2009. A meteor shower catalog based on video observations in 2007– 2008. WGN, Journal of the International Meteor Organization 37 (April), 55–62. Southworth, R.B., Hawkins, G.S., 1963. Statistics of meteor streams. In: Smithsonian Contributions to Astrophysics, vol. 7, p. 261. Vaubaillon, J., Colas, F., Jorda, L., 2005. A new method to predict meteor showers. I. Description of the model. Astron. Astrophys. 439 (August), 751–760. http://dx. doi.org/10.1051/0004-6361:20041544. Wiegert, P., Brown, P., 2004. The problem of linking minor meteor showers to their parent bodies: initial considerations. Earth Moon Planets 95 (December), 19–26. http://dx.doi.org/10.1007/s11038-005-4342-8.
Please cite this article as: Rudawska, R., Vaubaillon, J., Don Quixote—A possible parent body of a meteor shower. Planetary and Space Science (2015), http://dx.doi.org/10.1016/j.pss.2015.04.014i
Contents lists available at ScienceDirect
Planetary and Space Science journal homepage: www.elsevier.com/locate/pss
Don Quixote—A possible parent body of a meteor shower Regina Rudawska a,n, Jeremie Vaubaillon b a b
Comenius University, Faculty of Mathematics, Physics and Informatics, Mlynská dolina, Bratislava SK-84248, Slovakia Institut de Mécanique Céleste et de Calcul des Éphémérides - Observatoire de Paris, 77 avenue Denfert-Rochereau, 75014 Paris, France
art ic l e i nf o
a b s t r a c t
Article history: Received 22 January 2015 Received in revised form 13 April 2015 Accepted 22 April 2015
Asteroid 3552 Don Quixote (1983 SA) orbits the Sun on an orbit that resembles that of a short-period comet. This, together with its recently observed cometary activity, makes it a good candidate for a parent body of a meteor shower. Model calculations show that the particles originated from Don Quixote pass close enough to Earth orbit to search for a meteor shower activity. Corresponding meteor showers were found in CAMS (Rudawska and Jenniskens, 2014) and EDMOND (Kornoš et al., 2014) video observations. The κ Lyrids and August μ Draconids (IAU#464 and IAU#470, respectively), a similarly inclined stream active in the summer, are associated with 3552 Don Quixote. & 2015 Elsevier Ltd. All rights reserved.
Keywords: Meteor shower Meteoroid stream Comet Asteroid
1. Introduction Meteoroid streams originate during processes that occur on a surface of a comet (when it approaches the Sun) or on a surface of an asteroid (e.g. when asteroids collide). After abandoning the parent body, meteoroids start their journey in space, occupying similar orbits that creates a structure called meteoroid stream. When particles of the stream enter the Earth's atmosphere, they create phenomena called meteor shower. A given parent body can give origin to more than one meteor shower; e.g. 1P/Halley is a parent body of the Orionids and η Aquarids (Babadzhanov et al., 2008; Wiegert and Brown, 2004; Brown et al., 2008, 2010, Neslušan et al., 2014a,b, Rudawska et al., 2012; Rudawska and Jenniskens, 2014). Parent bodies also create dynamical groups (Asher et al., 1993; Babadzhanov, 2001), and give origin to complex meteoroid streams (e.g. Taurids complex. There are also NEAs thought to be extinct cometary nuclei, but which start to show cometary activity (Jewitt, 2012). Automated surveys of Near-Earth Objects (NEOs) continue to discover objects in cometary-like orbits that are likely candidate parent bodies. These have orbits with Tisserand parameters between 2 and 3, typical of Jupiter Family Comets. Some of those come close to Earth orbit, but are not associated with meteor shower activity. Here, we study the case of asteroid 3552 Don Quixote (1983 SA). At first there was no activity observed from Don Quixote when it n
Corresponding author. E-mail address: [email protected] (R. Rudawska).
approached the Sun. This was till recently when a tail was spotted from Don Quixote (Mommert et al., 2014). Asteroid (3552) Don Quixote was discovered in 1983 and categorized as Amor asteroid. It is an object of about 12.3–24.5 km diameter, low-albedo, spectral type D, and orbit which resembles that of a comet (the Tisserand parameter for the orbit has a value of 2.315 with respect to Jupiter). This observed activity makes Don Quixote a good candidate for a short-period comet among known NEOs. The question arises of whether a meteor shower can be created from Don Quixote? If so, do/did we observe it on Earth? In Section 2 we describe the method we applied. Section 3 focuses on the results, while Section 4 presents our conclusions.
2. Methodology In order to answer questions that arose in Section 1 our methodology combines two steps: meteoroid stream modelling, and search for similarity between the orbits of simulated stream and orbits of known meteoroid streams. Table 1 Orbital elements of 3552 Don Quixote (1983 SA). Source: JPL HORIZONS website.
q (AU)
e
i (deg)
ω (deg)
Ω (deg)
1.2099
0.71324
30.98
317.03
350.27
http://dx.doi.org/10.1016/j.pss.2015.04.014 0032-0633/& 2015 Elsevier Ltd. All rights reserved.
Please cite this article as: Rudawska, R., Vaubaillon, J., Don Quixote—A possible parent body of a meteor shower. Planetary and Space Science (2015), http://dx.doi.org/10.1016/j.pss.2015.04.014i
R. Rudawska, J. Vaubaillon / Planetary and Space Science ∎ (∎∎∎∎) ∎∎∎–∎∎∎
2
Table 2 Geocentric and orbital parameters of κ Lyrids and August μ Draconids. Source: IAU MDC. Stream
λ⊙ (deg)
α (deg)
δ (deg)
Vg (km/s)
q (AU)
e
ω (deg)
Ω (deg)
i (deg)
#464 KLY #470 AMD
126.9 145.4
277.5 253.7
þ 33.3 þ 58.8
18.6 19.5
0.939 1.011
0.698 0.654
215.1 177.2
126.8 145.4
24.7 30.3
3. Results
Table 3 Mean orbital elements of simulated meteoroid stream.
3.1. Possibly associated meteor showers q (AU)
e
ω (deg)
Ω (deg)
i (deg)
0.981
0.680
197.4
144.1
28.3
2.1. Meteoroid stream modelling We have investigated the orbital evolution of the meteoroid stream originating from Don Quixote asteroid. For this purpose we modelled the meteoroid stream originated from Don Quixote and its evolution in the Solar System. The model of generation and evolution of meteoroid stream in the solar system is taken from Vaubaillon et al. (2005). The initial orbital elements and physical properties of the object are taken from JPL HORIZONS website1 (Table 1), and integrated over an arc of orbit within three astronomical units. Each time the object approached the Sun, meteoroids were released at regular time intervals (one day) within 3 AU from the Sun. Ejection in a hemisphere towards the Sun is assumed with mass-dependent velocities taken from Crifo and Rodionov (1997). The ejections of 5000 meteoroids from the object's surface took place every 100 years when it was passing its perihelion between 5000 B.C. and 2013 A.D. Next, the orbits of the ejected meteoroids were integrated to year 2050 A.D. For this purpose, we used a 15th order Radau integrator (Everhart, 1985), while meteoroid orbits were controlled by gravitational and nongravitational forces (radiation pressure, Poynting–Robertson drag, and Yarkovky's effect). If a meteoroid is sufficiently close to the Earth, its orbital parameters are saved and compared with known showers. The theoretical radiant of a meteoroid orbit that passed within 0.05 AU from Earth is calculated with the Q method (Hasegawa, 1990) using Neslusan et al. (1998) software, which adjusts for the miss-distance by changing the perihelion distance. 2.2. Similarity functions The similarity between the orbits of the particles reaching the Earth with orbits of known meteoroid streams listed at the International Astronomical Union Meteor Data Center (IAU MDC) needs to be quantified. Many tests have been proposed to measure the difference between orbits and have recently been discussed in Jopek and Williams (2013). The most popular is that of Southworth and Hawkins (1963), but we choose to use the newer and more robust criterion of Jopek et al. (2008) described by heliocentric vectorial elements, namely
DV2 = wh1 (hB1 − hA1 )2 + wh2 (hB2 − hA2 )2 + 1.5 wh3 (hB3 − hA3 )2 + we1 (eB1 − eA1 )2 + we2 (eB2 − eA2 )2 + we3 (eB3 − eA3 )2 + 2wE (EB + EA )2 ,
(1)
where h A and h B are the angular momenta, e A and eB are the Laplace vectors, EA and EB are the orbital energy of two orbits, and w are weight coefficients. In the survey, we used values of weight coefficients taken from Jopek et al. (2008). 1
http://ssd.jpl.nasa.gov/?horizons
Using the method described in the previous section we found two meteor showers: κ Lyrids (#464, KLY), and August μ Draconids (#470, AMD). Both meteor showers remain on the working list of the IAU MDC2 (Table 2). κ Lyrids and August μ Draconids meteor showers were first identified in a cluster analysis applied to the combined meteoroid orbit database derived from low-light level video observations by the SonotaCo consortium in Japan (SonotaCo, 2009) and by the Cameras for All-sky Meteor Surveillance (CAMS; Jenniskens et al., 2011) project in California, USA (Rudawska and Jenniskens (2014). AMD shower consisted 6 orbits, where 5 of them were meteors detected by CAMS. In case of KLY meteor shower, 5 out of 6 meteors were observed by SonotaCo. Kornoš et al. (2014), using the radiant position-geocentric velocity method, also identified those showers in the 4th version of the EDMOND database (Kornos et al., 2013). We compare the orbits of κ Lyrids and August μ Draconids (Table 2) with orbits from our simulation (Table 3), using DV, we achieved a good match. The obtained values of DV for KLY and AMD meteor showers (0.05 and 0.05, respectively) are below conventional threshold value assumed when establishing orbits similarity, i.e. 0.08 (Jopek et al., 2008; Rudawska et al., 2012). 3.2. Radiants' distribution In Fig. 1, we compare all modelled meteors with observed κ Lyrids and August μ Draconids meteor showers. The theoretical radiant of a meteoroid orbit that passed sufficiently close to Earth is calculated with the Q method (Hasegawa, 1990). The distribution of theoretical radiant plotted together with radiant position of KLY and AMD taken from the IAU MDC as well as with KLY and AMD identified by independent identification method applied to the latest version of the EDMOND database (Rudawska et al., 2014). The position of both showers taken from the IAU MDC nicely fits the simulated meteor shower, occupying two parts of the simulated shower. Moreover, when we add members of both meteor showers found in the EDMOND database by the independent method, we notice that the observed dispersion of radiants is in excellent agreement with the simulated distribution.
4. Conclusion This paper addresses the topic of the meteoroid stream of a parent body in relation to meteor showers observed on Earth. We carried out a search to investigate the possibility of meteor shower observations caused by particles ejected from 3552 Don Quixote (1983 SA). We showed that if Don Quixote did eject a meteoroid stream in the past 5000 years, it would produce meteor showers on Earth today that match the observed κ Lyrids and μ Draconids. This is a 2
http://www.astro.amu.edu.pl/ jopek/MDC2007/
Please cite this article as: Rudawska, R., Vaubaillon, J., Don Quixote—A possible parent body of a meteor shower. Planetary and Space Science (2015), http://dx.doi.org/10.1016/j.pss.2015.04.014i
R. Rudawska, J. Vaubaillon / Planetary and Space Science ∎ (∎∎∎∎) ∎∎∎–∎∎∎
Fig. 1. Radiant position for simulated meteor shower ( ), κ Lyrids ( ) and August μ Draconids ( ) taken from IAU MDC (Table 2), and κ Lyrids ( ) and August μ Draconids ( ) identified in EDMOND database by Rudawska et al. (2014).
necessary step towards the association between these showers and Don Quixote. A total of 11 orbits of κ Lyrids and August μ Draconids from IAU MDC were taken into account in this study. Future additional orbital data would be extremely useful to definitely prove without ambiguity the parenthood of Don Quixote with these two showers.
References Asher, D.J., Clube, S.V.M., Steel, D.I., 1993. Asteroids in the Taurid complex. Mon. Not. R. Astron. Soc. 264 (September), 93. Babadzhanov, P.B., 2001. Search for meteor showers associated with Near-Earth Asteroids. I. Taurid Complex. Astron. Astrophys. 373 (July), 329–335. http://dx. doi.org/10.1051/0004-6361:20010583. Babadzhanov, P.B., Williams, I.P., Kokhirova, G.I., 2008. Meteor showers associated with 2003EH1. Mon. Not. R. Astron. Soc. 386 (June), 2271–2277. http://dx.doi. org/10.1111/j.1365-2966.2008.13202.x. Brown, P., Weryk, R.J., Wong, D.K., Jones, J., 2008. A meteoroid stream survey using the Canadian Meteor Orbit Radar. I. Methodology and radiant catalogue. Icarus 195 (May), 317–339. http://dx.doi.org/10.1016/j.icarus.2007.12.002. Brown, P., Wong, D.K., Weryk, R.J., Wiegert, P., 2010. A meteoroid stream survey using the Canadian Meteor Orbit Radar. II: Identification of minor showers using a 3D wavelet transform. Icarus 207 (May), 66–81. http://dx.doi.org/ 10.1016/j.icarus.2009.11.015.
3
Crifo, J.F., Rodionov, A.V., 1997. The dependence of the circumnuclear coma structure on the properties of the nucleus. Icarus 127 (June), 319–353. http://dx.doi. org/10.1006/icar.1997.5690. Everhart, E., 1985. An efficient integrator that uses Gauss–Radau spacings. In: Carusi, A., Valsecchi, G.B. (Eds.), Dynamics of Comets: Their Origin and Evolution, Proceedings of IAU Colloq. 83, held in Rome, Italy, June 11–15, 1984, Astrophysics and Space Science Library, vol. 115. Riedel, Dordrecht, 1985, p. 185. Hasegawa, I., 1990. Predictions of the meteor radiant point associated with a comet. Astron. Soc. Jpn. 42 (February), 175–186. Jenniskens, P., Gural, P.S., Dynneson, L., Grigsby, B.J., Newman, K.E., Borden, M., Koop, M., Holman, D., 2011. CAMS: Cameras for Allsky Meteor Surveillance to establish minor meteor showers. Icarus 216 (November), 40–61. http://dx.doi. org/10.1016/j.icarus.2011.08.012. Jewitt, D., 2012. The active asteroids. Astron. J. 143 (March), 66. http://dx.doi.org/ 10.1088/0004-6256/143/3/66. Jopek, T.J., Rudawska, R., Bartczak, P., 2008. Meteoroid stream searching: the use of the vectorial elements. Earth Moon Planets 102 (June), 73–78. http://dx.doi.org/ 10.1007/s11038-007-9197-8. Jopek, T.J., Williams, I.P., 2013. Stream and sporadic meteoroids associated with near-Earth objects. Mon. Not. R. Astron. Soc. 430 (April), 2377–2389. http://dx. doi.org/10.1093/mnras/stt057. Kornos, L., Koukal, J., Piffl, R., Toth, J., 2013. Database of meteoroid orbits from several European video networks. In: Gyssens, M., Roggemans, P. (Eds.), Proceedings of the International Meteor Conference, 31st IMC, La Palma, Canary Islands, Spain, 2012, January, pp. 21–25. Kornoš, L., Matlovič, P., Rudawska, R., Tóth, J., Hajduková, M., Koukal, J., Piffl, R., 2014. Confirmation and characterization of IAU temporary meteor showers in EDMOND database. ArXiv e-prints, May. Mommert, M., Hora, J.L., Harris, A.W., Reach, W.T., Emery, J.P., Thomas, C.A., Mueller, M., Cruikshank, D.P., Trilling, D.E., Delbo, M., Smith, H.A., 2014. The discovery of cometary activity in near-earth asteroid (3552) Don Quixote. Astrophys. J. 781 (January), 25. http://dx.doi.org/10.1088/0004-637X/781/1/25. Neslusan, L., Svoren, J., Porubcan, V., 1998. A computer program for calculation of a theoretical meteor-stream radiant. Astron. Astrophys. 331 (March), 411–413. Neslušan, L., Hajduková, M., Tomko, D., Kaňuchová, Z., Jakubík, M., 2014a. The prediction of meteor showers from all potential parent comets. In: Rault, J.-L., Roggemans, P. (Eds.), Proceedings of the International Meteor Conference, Giron, France, 18–21 September 2014, February, pp. 139–145. Neslušan, L., Kaňuchová, Z., Tomko, D., 2014b. The ecliptic-toroidal structure of the meteor complex of comet 96P/Machholz. Meteoroids 2013 (July), 235–242. Rudawska, R., Jenniskens, P., 2014. New meteor showers identified in the CAMS and SonotaCo meteoroid orbit surveys. Meteoroids 2013 (July), 217–224. Rudawska, R., Matlovič, P., Tóth, J., Kornoš, L., 2014. Independent identification of meteor showers in EDMOND database. In: Rault, J.-L., Roggemans, P. (Eds.), Proceedings of the International Meteor Conference, Giron, France, 18–21 September 2014, February, pp. 98–100. Rudawska, R., Vaubaillon, J., Atreya, P., 2012. Association of individual meteors with their parent bodies. Astron. Astrophys. 541 (May), A2. http://dx.doi.org/10.1051/ 0004-6361/201118762. SonotaCo, 2009. A meteor shower catalog based on video observations in 2007– 2008. WGN, Journal of the International Meteor Organization 37 (April), 55–62. Southworth, R.B., Hawkins, G.S., 1963. Statistics of meteor streams. In: Smithsonian Contributions to Astrophysics, vol. 7, p. 261. Vaubaillon, J., Colas, F., Jorda, L., 2005. A new method to predict meteor showers. I. Description of the model. Astron. Astrophys. 439 (August), 751–760. http://dx. doi.org/10.1051/0004-6361:20041544. Wiegert, P., Brown, P., 2004. The problem of linking minor meteor showers to their parent bodies: initial considerations. Earth Moon Planets 95 (December), 19–26. http://dx.doi.org/10.1007/s11038-005-4342-8.
Please cite this article as: Rudawska, R., Vaubaillon, J., Don Quixote—A possible parent body of a meteor shower. Planetary and Space Science (2015), http://dx.doi.org/10.1016/j.pss.2015.04.014i