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J/A+A/603/A72       R light curves of MN Dra                 (Bakowska+, 2017)

MN Draconis: a peculiar, active dwarf nova in the period gap. Bakowska K., Olech A., Pospieszynski R., Swierczynski E., Martinelli F., Rutkowski A., Koff R., Drozd K., Butkiewicz-Bak M., Kankiewicz P. <Astron. Astrophys. 603, A72 (2017)> =2017A&A...603A..72B (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, cataclysmic ; Novae ; Photometry Keywords: binaries (including multiple): close - stars: individual: MN Draconis - novae, cataclysmic variables - stars: dwarf novae Abstract: We present results of an extensive world-wide observing campaign of MN Draconis. MN Draconis is a poorly known active dwarf nova in the period gap and is one of the only two known cases of period gap SU UMa objects showing the negative superhumps. Photometric behaviour of MN Draconis poses a challenge for existing models of the superhump and superoutburst mechanisms. Therefore, thorough investigation of peculiar systems, such as MN Draconis, is crucial for our understanding of evolution of the close binary stars. To measure fundamental parameters of the system, we collected photometric data in October 2009, June-September 2013 and June-December 2015. Analysis of the light curves, O-C diagrams and power spectra was carried out. 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 Psc=74±0.5-days and it has been increasing with a rate of Pdot=3.3x10-3 during last 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 in result, the orbital period Porb=0.0994(1)days (143.126±0.144min). We updated the basic light curve parameters of MN Draconis. MN Draconis is the first discovered SU UMa system in the period gap with increasing supercycle length. Description: The observational data of MN Dra presented here were collected throughout three observation campaigns. The first data were obtained during 6 nights from 2009 October 12 to October 22, in the Skinakas Observatory, Greece. At that time, the star was in a quiescent state. The second campaign was conducted during 15 nights from 2013 July 09 to September 10. On that occasion, data were gathered in Poland, at the Borowiec station of the Poznan Astronomical Observatory, at J. Kochanowski University in Kielce, and at the Ostrowik station of theWarsaw University Observatory. During the 2013 campaign we detected two superoutbursts of MN Dra. The longest campaign was organized in 2015, from June 4 to December 18. Data covering 84 nights of observations were collected at the Borowiec Station, in Pisa in Italy, at Antelope Hills Observatory and at the MDM Observatory in the USA. Once again, two superoutbursts inMN Dra were observed. R broad-band photometry of MN Dra was obtained in three runs organized in 2009 (table 2009.dat), 2013 (table 2013.dat) and 2015 (table 2015.dat). Objects: -------------------------------------------- RA (2000) DE Designation(s) -------------------------------------------- 20 23 38.146 +64 36 27.19 MN Dra = V73 Dra -------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file 2009.dat 35 371 R photometry of MN Dra from 2009 2013.dat 35 2564 R photometry of MN Dra from 2013 2015.dat 35 5187 R photometry of MN Dra from 2015
Byte-by-byte Description of file: 2009.dat 2013.dat 2015.dat
Bytes Format Units Label Explanations
1- 16 F16.8 d HJD Helicentric Julian Date 18- 24 F7.4 mag Rmag R magnitude 26- 35 F10.8 mag e_Rmag rms uncertainty on Rmag
Acknowledgements: Karolina Bakowska, bakowska(at)camk.edu.pl
(End) Patricia Vannier [CDS] 27-Mar-2017
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