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Variations in the Period of Negative Superhumps in SU UMa-Type Dwarf Novae. I. Mn Dra (2012-2017)

Sklyanov A.S., Pavlenko E.P., Antonyuk K.A., Pit N.V., Malanushenko V.P., Shchurova A.V., Zaostrozhnykh A.M.A., Shugarov S.Y., Sosnovskij A.A., Babina J.V., Antonyuk O.I., Simon A.O., Zhuchkov R.Y., Gutaev A.G.

observed and in the quiescent state, negative superhumps with an average period of 0.095921(3) days

NY Ser: Outburst Activity and Multiperiodic Processes in its Various Stages During 2014 and 2016

the superoutburst we identified two stages in the evolution of superhumps: a stage in which the tidal instability

Survey of period variations of superhumps in SU UMa-type dwarf novae. VI. The sixth year (2013-2014)

Kato T., Dubovsky P., Kudzej I., Hambsch F., Miller I., Ohshima T., Nakata C., Kawabata M., Nishino H., Masumoto K., Mizoguchi S., Yamanaka M., Matsumoto K., Sakai D., Fukushima D., Matsuura M., Bouno G., Takenaka M., Nakagawa S., Noguchi R., Iino E., Pickard R., Maeda Y., Henden A., Kasai K., Kiyota S., Akazawa H., Imamura K., De Miguel E., Maehara H., Monard B., Pavlenko E., Antonyuk K., Pit N., Antonyuk O., Baklanov A., Ruiz J., Richmond M., Oksanen A., Harlingten C., Shugarov S., Chochol D., Masi G., Nocentini F., Schmeer P., Bolt G., Nelson P., Ulowetz J., Sabo R., Goff W., Stein W., Michel R., Dvorak S., Voloshina I., Metlov V., Katysheva N., Neustroev V., Sjoberg G., Littlefield C., Dębski B., Sowicka P., Klimaszewski M., Curyło M., Morelle E., Curtis I., Iwamatsu H., Butterworth N., Andreev M., Parakhin N., Sklyanov A., Shiokawa K., Novák R., Irsmambetova T., Itoh H., Ito Y., Hirosawa K., Denisenko D., Kochanek C., Shappee B., Stanek K., Prieto J., Itagaki K., Stubbings R.

and characterized these objects. We detected negative superhumps in VW Hyi and indicated that the low number

Survey of period variations of superhumps in SU UMa-type dwarf novae. VI. The sixth year (2013-2014)

Kato T., Dubovsky P., Kudzej I., Hambsch F., Miller I., Ohshima T., Nakata C., Kawabata M., Nishino H., Masumoto K., Mizoguchi S., Yamanaka M., Matsumoto K., Sakai D., Fukushima D., Matsuura M., Bouno G., Takenaka M., Nakagawa S., Noguchi R., Iino E., Pickard R., Maeda Y., Henden A., Kasai K., Kiyota S., Akazawa H., Imamura K., De Miguel E., Maehara H., Monard B., Pavlenko E., Antonyuk K., Pit N., Antonyuk O., Baklanov A., Ruiz J., Richmond M., Oksanen A., Harlingten C., Shugarov S., Chochol D., Masi G., Nocentini F., Schmeer P., Bolt G., Nelson P., Ulowetz J., Sabo R., Goff W., Stein W., Michel R., Dvorak S., Voloshina I., Metlov V., Katysheva N., Neustroev V., Sjoberg G., Littlefield C., Dębski B., Sowicka P., Klimaszewski M., Curyło M., Morelle E., Curtis I., Iwamatsu H., Butterworth N., Andreev M., Parakhin N., Sklyanov A., Shiokawa K., Novák R., Irsmambetova T., Itoh H., Ito Y., Hirosawa K., Denisenko D., Kochanek C., Shappee B., Stanek K., Prieto J., Itagaki K., Stubbings R.

and characterized these objects. We detected negative superhumps in VW Hyi and indicated that the low number

Long-period SUUMa dwarf nova V1006 Cygni: Outburst activity and variability at different brightness states in 2015 - 2017

Godunova V., Sokolov I., Rudakov I.

and the second normal outbursts in 2015 we possibly detected the negative superhumps with the period of 0d:09714

Superhump evolution of WZ Sge-type dwarf nova ASASSN-14cv at rebrightening stage

Sklyanov A., Pavlenko E., Antonyuk O., Antonyuk K., Sosnovsky A., Galeev A., Pit’ N., Babina Y.

superhump evolution can be either described by a parabolic approximation with the negative Pdot = −1.1 × 10

Superhump evolution of WZ Sge-type dwarf nova ASASSN-14cv at rebrightening stage

Sklyanov A., Pavlenko E., Antonyuk O., Antonyuk K., Sosnovsky A., Galeev A., Pit’ N., Babina Y.

superhump evolution can be either described by a parabolic approximation with the negative Pdot = −1.1 × 10

Disk precession and quasi-periodic brightness oscillations of V603 Aql in 2001-2002

Suleimanov V., Bikmaev I., Belyakov K., Sakhibullin N., Zhukov G., Aslan Z., Kiziloglu U., Khamitov I.

with negative superhumps was found to be brighter than it is in a state with positive superhumps by 0.m2-0.m3

Disk precession and quasi-periodic brightness oscillations of V603 Aql in 2001-2002

Suleimanov V., Bikmaev I., Belyakov K., Sakhibullin N., Zhukov G., Aslan Z., Kiziloglu U., Khamitov I.

with negative superhumps was found to be brighter than it is in a state with positive superhumps by 0.m2-0.m3

MASTER OT J172758.09+380021.5: a peculiar ER UMa-type dwarf nova, probably a missed nova in the recent past

Pavlenko E., Kato T., Antonyuk K., Pit N., Keir L., Udovichenko S., Dubovský P., Sosnovskij A., Antonyuk O., Shimansky V., Gabdeev M., Rakhmatullaeva F., Kokhirova G., Belan S., Simon A., Baklanov A., Kojiguchi N., Godunova V.

by an orbital period of 0.057026 d or its orbital-negative superhump beat period were detected. An absence

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