Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · 1406.6428

Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. VI: The Sixth Year (2013-2014)

Taichi Kato·Pavol A. Dubovsky·Igor Kudzej·Franz-Josef Hambsch·Ian Miller·Tomohito Ohshima·Chikako Nakata·Miho Kawabata·Hirochika Nishino·Kazunari Masumoto·Sahori Mizoguchi·Masayuki Yamanaka·Katsura Matsumoto·Daisuke Sakai·Daiki Fukushima·Minami Matsuura·Genki Bouno·Megumi Takenaka·Shinichi Nakagawa·Ryo Noguchi·Eriko Iino·Roger D. Pickard·Yutaka Maeda·Arne Henden·Kiyoshi Kasai·Seiichiro Kiyota·Hidehiko Akazawa·Kazuyoshi Imamura·Enrique de Miguel·Hiroyuki Maehara·Berto Monard·Elena P. Pavlenko·Kirill Antonyuk·Nikolaj Pit·Oksana I. Antonyuk·Aleksei V. Baklanov·Javier Ruiz·Michael Richmond·Arto Oksanen·Caisey Harlingten·Sergey Yu. Shugarov·Drahomir Chochol·Gianluca Masi·Francesca Nocentini·Patrick Schmeer·Greg Bolt·Peter Nelson·Joseph Ulowetz·Richard Sabo·William N. Goff·William Stein·Raul Michel·Shawn Dvorak·Irina B. Voloshina·Vladimir Metlov·Natalia Katysheva·Vitaly V. Neustroev·George Sjoberg·Colin Littlefield·Bartlomiej Debski·Paulina Sowicka·Marcin Klimaszewski·Malgorzata Curylo·Etienne Morelle·Ivan A. Curtis·Hidetoshi Iwamatsu·Neil D. Butterworth·Maksim V. Andreev·Nikolai Parakhin·Aleksandr Sklyanov·Kazuhiko Shiokawa·Rudolf Novak·Tat'yana R. Irsmambetova·Hiroshi Itoh·Yoshiharu Ito·Kenji Hirosawa·Denis Denisenko·Christopher S. Kochanek·Benjamin Shappee·Krzysztof Z. Stanek·Jose L. Prieto·Koh-ichi Itagaki·Rod Stubbings·Jose Ripero·Eddy Muyllaert·Gary Poyner
View original source ↗Read source document ↗Export metadata ↓

Abstract

Continuing the project described by Kato et al. (2009, PASJ, 61, S395, arXiv:0905.1757), we collected times of superhump maxima for 56 SU UMa-type dwarf novae mainly observed during the 2013-2014 season and characterized these objects. We detected negative superhumps in VW Hyi and indicated that the low number of normal outbursts in some supercycle can be interpreted as a result of the disk tilt. This finding, combined with the Kepler observation of V1504 Cyg and V344 Lyr, suggests that the disk tilt is responsible for modulating the outburst pattern in SU UMa-type dwarf novae. We also studied the deeply eclipsing WZ Sge-type dwarf nova MASTER OT J005740.99+443101.5 and found evidence of a sharp eclipse during the phase of early superhumps. The profile can be reproduced by a combination of the eclipse of the axisymmetric disk and the uneclipsed light source of early superhumps. This finding confirms the lack of evince of a greatly enhanced hot spot during the early stage of WZ Sge-type outburst. We detected growing (stage A) superhumps in MN Dra and give a suggestion that some of SU UMa-type dwarf novae situated near the critical condition of tidal instability may show long-lasting stage A superhumps. The large negative period derivatives reported in such systems can be understood a result of the combination of stage A and B superhumps. The WZ Sge-type dwarf novae AL Com and ASASSN-13ck showed a long-lasting (plateau-type) rebrightening. In the early phase of the rebrightening, both objects showed a precursor-like outburst, suggesting that the long-lasting rebrightening is triggered by a precursor outburst.

Explore related subjects

astro-ph.SR

Keep this discovery

BibTeXRIS

Taichi Kato, Pavol A. Dubovsky, Igor Kudzej, Franz-Josef Hambsch, Ian Miller, Tomohito Ohshima, Chikako Nakata, Miho Kawabata, Hirochika Nishino, Kazunari Masumoto, Sahori Mizoguchi, Masayuki Yamanaka, Katsura Matsumoto, Daisuke Sakai, Daiki Fukushima, Minami Matsuura, Genki Bouno, Megumi Takenaka, Shinichi Nakagawa, Ryo Noguchi, Eriko Iino, Roger D. Pickard, Yutaka Maeda, Arne Henden, Kiyoshi Kasai, Seiichiro Kiyota, Hidehiko Akazawa, Kazuyoshi Imamura, Enrique de Miguel, Hiroyuki Maehara, Berto Monard, Elena P. Pavlenko, Kirill Antonyuk, Nikolaj Pit, Oksana I. Antonyuk, Aleksei V. Baklanov, Javier Ruiz, Michael Richmond, Arto Oksanen, Caisey Harlingten, Sergey Yu. Shugarov, Drahomir Chochol, Gianluca Masi, Francesca Nocentini, Patrick Schmeer, Greg Bolt, Peter Nelson, Joseph Ulowetz, Richard Sabo, William N. Goff, William Stein, Raul Michel, Shawn Dvorak, Irina B. Voloshina, Vladimir Metlov, Natalia Katysheva, Vitaly V. Neustroev, George Sjoberg, Colin Littlefield, Bartlomiej Debski, Paulina Sowicka, Marcin Klimaszewski, Malgorzata Curylo, Etienne Morelle, Ivan A. Curtis, Hidetoshi Iwamatsu, Neil D. Butterworth, Maksim V. Andreev, Nikolai Parakhin, Aleksandr Sklyanov, Kazuhiko Shiokawa, Rudolf Novak, Tat'yana R. Irsmambetova, Hiroshi Itoh, Yoshiharu Ito, Kenji Hirosawa, Denis Denisenko, Christopher S. Kochanek, Benjamin Shappee, Krzysztof Z. Stanek, Jose L. Prieto, Koh-ichi Itagaki, Rod Stubbings, Jose Ripero, Eddy Muyllaert, Gary Poyner. 2014-06-25. Survey of Period Variations of Superhumps in SU UMa-Type Dwarf Novae. VI: The Sixth Year (2013-2014). https://doi.org/10.1093/pasj/psu072

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Eclipse Properties and Superhump Evolution in the SU UMa-Type Dwarf Nova Z Cha

The advent of large-scale time-domain surveys provides both opportunities and challenges for understanding accretion disk evolution in cataclysmic variables (CVs). Using high-cadence photometry from the Transiting Exoplanet Survey Satellite (TESS), we investigate the eclipsing SU UMa-type dwarf nova Z Cha. Leveraging eclipses as a natural probe, we examine the evolution of the accretion disk through variations in eclipse depth, O--C of eclipse minima, and positive superhump (PSH) amplitude. During superoutbursts, all three quantities exhibit quasi-periodic modulations with a common period of $\sim$2 days, consistent with the precession period of an eccentric disk. We interpret these correlated variations as evidence of an eccentric, precessing disk: O--C traces the periodic shift of the system's brightness center, while eclipse depth and PSH amplitude vary with the orientation of the disk bulge relative to the line of sight. In quiescence (Sectors 13 and 93), PSHs with periods of $\sim$0.0762 days show linearly decreasing amplitudes and periods, indicating gradual shrinkage of the eccentric disk and a slowing precession. Remarkably, a coherent signal with a period of $\sim$0.0729~days ($\epsilon^{-}\approx-0.02$) appears in the same quiescent intervals. This signal may represent negative superhumps (NSHs) coexisting with PSHs, although an orbital sideband of the PSH cannot presently be excluded with the available data. If confirmed as NSHs, their coexistence with PSHs would challenge the classical tilted-disk model, and could be explained by retrograde apsidal precession of an eccentric disk, where the inner disk precesses retrogradely (NSHs) and the outer disk progradely (PSHs); this interpretation remains to be tested by further observations.

astro-ph.SR↗
arXiv2026

Classical Nova V1405 Cas Had $M_{\rm ejecta}$$>$$M_{\rm accreted}$ and so is Unlikely to be a Type Ia Supernova Progenitor

Nova 2021 Cassiopeia (V1405 Cas) was an ordinary J(175) neon nova with the white dwarf mass estimated to be $M_{\rm WD}$=0.60$\pm$0.10 $M_{\odot}$. I found an orbital period of $P$=0.1884 days, and have tracked 20 times of photometric minima from 2013--2025. I measure that $P$ increased from before to after the eruption with $P_{\rm pre}$=0.1883919$\pm$0.0000018 days and $P_{\rm post}$=0.1884043$\pm$0.0000018 days, for $\Delta P$/$P$=66$_{-18}^{+21}$ parts-per-million. With correction for the angular momentum loss by the binary during the eruption, I derive that the nova ejected $M_{\rm ejecta}$=7.5$\times$10$^{-4}$ $M_{\odot}$, with an extreme range of (2.9--40)$\times$10$^{-4}$ $M_{\odot}$. The mass accreted during the previous eruption cycle comes from the trigger mass, and is $M_{\rm accreted}$=(1.6$\pm$0.4)$\times$10$^{-4}$ $M_{\odot}$. V1405 Cas provides counterexamples against five claims about CV evolution that have dominated since the 1980s. First, V1405 Cas has positive $\dot{P}$, and this is contrary to the Magnetic Braking Model. Second, the $\Delta P$ is 20$\times$ too small to allow the system to fade into a hibernation state. Third, $M_{\rm WD}$ is decreasing over time, as shown by $M_{\rm ejecta}$$>$$M_{\rm accreted}$ and by being a neon nova. Fourth, V1405 Cas is not a Type Ia supernova progenitor, for the same reasons. Fifth, the orbital period of V1405 Cas increased by $+$75 ppm from 2013--2025, as a counterexample to the pervasive idea that cataclysmic variables are universally declining in period from evolution. V1405 Cas is the latest of recent measures of $\Delta P$ and $\dot{P}$ for 52 cataclysmic variables and 25 X-ray binaries that have together refuted all five claims.

astro-ph.SR↗
arXiv2026

A prolonged plateau-to-tail transition in the Type II supernova SN2025abyc

We present optical photometric and spectroscopic observations of the Type II supernova SN2025abyc. During the optically thick phase between approximately 10 and 70 d after explosion, its light curves show strongly wavelength-dependent decline rates of approximately 2.7, 2.1, 0.9, and 0.8 mag/100d in the g, c, r, and o bands, respectively. At approximately 70 d, the light curves begin to depart from their nearly linear plateau evolution and gradually transition toward the radioactive tail. A Fermi-Dirac fit to the well-sampled ATLAS o-band light curve yields a transition midpoint of t_PT ~ 100.5d. The interval between the end of the linear plateau and this transition midpoint is approximately 30 d, indicating a prolonged plateau-to-tail transition. This timescale is comparable to those measured for SN2013by, SN2013ej, and SN2014G. Spectroscopically, at +13 d post-explosion, the Halpha profile appears weak and broad, whereas Hbeta and Hgamma display clear P-Cygni profiles. This morphology can be explained by the normal early spectroscopic evolution of SNe II, although partial filling of the Halpha absorption trough by emission associated with circumstellar interaction cannot be excluded. SN2025abyc otherwise follows the general photospheric velocity evolution of SNe II, while remaining toward the high-velocity side of the comparison distribution in Halpha, Hbeta, and FeII. Exploratory light-curve modelling suggests a synthesized Ni mass of approximately 0.03-0.04 solar mass. We suggest that the extended circumstellar environment, Ni distribution, and hydrogen-envelope structure could all play a role in shaping the observed light-curve evolution, particularly the prolonged plateau-to-tail transition.

astro-ph.SR↗