Comets and Meteors Workshop

Warsaw, Poland

Comets and Meteors Workshop

Warsaw, Poland
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Bakowska K.,Polish Academy of Sciences | Olech A.,Polish Academy of Sciences | Pospieszynski R.,Comets and Meteors Workshop | Swierczynski E.,Nicolaus Copernicus University | And 6 more authors.
Astronomy and Astrophysics | Year: 2017

Context. We present results of an extensive world-wide observing campaign of MN Draconis. Aims. MN Draconis is a poorly known active dwarf nova in the period gap and is one of only two known cases of period-gap SU UMa objects showing negative superhumps. The photometric behaviour of MN Draconis poses a challenge for existing models of the superhump and superoutburst mechanisms. Therefore, a thorough investigation of peculiar systems like MN Draconis is crucial for our understanding of the evolution of close binary stars. Methods. To measure the fundamental parameters of the system, we collected photometric data in October 2009, June-September 2013, and June-December 2015. We analysed the light curves, O-C diagrams, and power spectra. Results. During our three observational seasons we detected four superoutburts and several normal outbursts. Based on the two consecutive superoutbursts detected in 2015, the supercycle length was derived as Psc = 74 ± 0.5 days, and it has been increasing with a rate of P = 3.3 × 10-3 during the past twelve years. Based on the positive and negative superhumps, we calculated the period excess ϵ = 5.6% ± 0.1%, the period deficit ϵ- = 2.5% ± 0.6%, and as a result, the orbital period Porb = 0.0994(1) days (143.126 ± 0.144 min). We updated the basic light curve parameters of MN Draconis. Conclusions. MN Draconis is the first discovered SU UMa system in the period gap with an increasing supercycle length. © ESO, 2017.


Olech A.,Nicolaus Copernicus Astronomical Center | Zoladek P.,Comets and Meteors Workshop | Tyminski Z.,Narodowe Centrum Badan Jadrowych | Stolarz M.,Comets and Meteors Workshop | And 6 more authors.
Contributions of the Astronomical Observatory Skalnate Pleso | Year: 2017

On September 12, 2016, at 21:44:07 UT, a -9.2 ± 0.5 mag fireball appeared over northeastern Poland. The precise orbit and atmospheric trajectory of the event are presented, based on the data collected by six video stations of the Polish Fireball Network (PFN). The PF120916 Piecki fireball entered the Earth's atmosphere with the velocity of 16.7 ± 0.3 km/s and started to shine at a height of 81.9 ± 0.3 km. Clear deceleration started after first three seconds of the flight, and the terminal velocity of the meteor was only 5.0 ± 0.3 km/s at a height of 26.0 ± 0.2 km. Such a low value of the terminal velocity indicates that fragments with the total mass of around 10 - 15 kg could survive the atmospheric passage and cause fall of the meteorites. The predicted area of possible meteorite impact is computed and it is located south of Reszel city at the Warmian-Masurian region. The impact area was extensively searched by experienced groups of meteorite hunters, but without any success.


Olech A.,Polish Academy of Sciences | Zoladek P.,Comets and Meteors Workshop | Wisniewski M.,Comets and Meteors Workshop | Rudawska R.,European Space Agency | And 9 more authors.
Monthly Notices of the Royal Astronomical Society | Year: 2016

On the night of October 31, 2015 two bright Southern Taurid fireballs occurred over Poland, being one of the most spectacular bolides of this shower in recent years. The first fireball - PF311015a Okonek - was detected by six video stations of Polish Fireball Network (PFN) and photographed by several bystanders, allowing for precise determination of the trajectory and orbit of the event. The PF311015a Okonek entered Earth's atmosphere with the velocity of 33.2 ± 0.1 km s-1 and started to shine at height of 117.88 ± 0.05 km. The maximum brightness of -16.0 ± 0.4 mag was reached at height of 82.5 ± 0.1 km. The trajectory of the fireball ended at height of 60.2 ± 0.2 km with terminal velocity of 30.2 ± 1.0 km s-1. The second fireball - PF311015b Ostrowite - was detected by six video stations of PFN. It started with velocity of 33.2 ± 0.1 km s-1 at height of 108.05 ± 0.02 km. The peak brightness of -14.8 ± 0.5 mag was recorded at height of 82.2 ± 0.1 km. The terminal velocity was 31.8 ± 0.5 km s-1 and was observed at height of 57.86 ± 0.03 km. The orbits of both fireballs are similar not only to orbits of Southern Taurids and comet 2P/Encke, but even closer resemblance was noticed for orbits of 2005 UR and 2005 TF50 asteroids. Especially the former object is interesting because of its close flyby during spectacular Taurid maximum in 2005. We carried out a further search to investigate the possible genetic relationship of Okonek and Ostrowite fireballs with both asteroids, that are considered to be associated with Taurid complex. Although, we could not have confirmed unequivocally the relation between fireballs and these objects, we showed that both asteroids could be associated, having the same origin in a disruption process that separates them. © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.


Olech A.,Polish Academy of Sciences | Zoladek P.,Comets and Meteors Workshop | Wisniewski M.,Comets and Meteors Workshop | Fietkiewicz K.,Comets and Meteors Workshop | And 8 more authors.
Astronomy and Astrophysics | Year: 2013

On the night of Oct. 18/19, 2012, at 00:23 UT, a -14.7 mag Orionid fireball occurred over northeastern Poland. The precise orbit and atmospheric trajectory of the event are presented, based on the data collected by five video stations and one photographic Polish Fireball Network station. The beginning height of the meteor is 168.4 ± 0.6 km, which makes the PF191012 Myszyniec fireball the highest ever observed, well-documented meteor not belonging to the Leonid shower. The ablation became the dominant source of light of the meteor at a height of around 115 km. The thermalization of sputtered particles is suggested to be the source of radiation above that value. The transition height of 115 km is 10-15 km below the transition heights derived for Leonids and might suggest that the material of Leonids is more fragile and probably has smaller bulk density than that of Orionids. © ESO, 2013.


Bakowska K.,Polish Academy of Sciences | Olech A.,Polish Academy of Sciences | Pospieszynski R.,Comets and Meteors Workshop | Martinelli F.,Lajatico Astronomical Center | Marciniak A.,Adam Mickiewicz University
Acta Astronomica | Year: 2014

Results of the CCD observations of CzeV404 are presented. During the season of June-August 2014 we detected one outburst and one superoutburst of the star. Clear superhumps with the period of Psh = 0.10472(2) days were observed. The superhump period was decreasing with a high value of P= -2.43(8) × 10-4. From 17 eclipses we calculated the orbital period with the value of Porb = 0.0980203(6) days which confirms that CzeV404 belongs to period gap objects and it is the longest orbital period of an eclipsing SU UMa star. Based on superhump and orbital period determinations, the period excess ε = 6.8% ± 0.02% and the mass ratio q ≈ 0.32 of the system were obtained.

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