Survey of period variations of superhumps in su UMa-type dwarf novae

被引：0

作者：

Kato, Taichi ^{[1
]}

Imada, Akira ^{[2
]}

Uemura, Makoto ^{[3
]}

Nogami, Daisaku ^{[4
]}

Maehara, Hiroyuki ^{[4
]}

Ishioka, Ryoko ^{[5
]}

Baba, Hajime ^{[6
]}

Matsumoto, Katsura ^{[7
]}

Iwamatsu, Hidetoshi ^{[1
]}

Kubota, Kaori ^{[1
]}

Sugiyasu, Kei ^{[1
]}

Soejima, Yuichi ^{[1
]}

Moritani, Yuuki ^{[1
]}

Ohshima, Tomohito ^{[1
]}

Ohashi, Hiroyuki ^{[1
]}

Tanaka, Junpei ^{[1
]}

Sasada, Mahito ^{[3
]}

Arai, Akira ^{[3
]}

Nakajima, Kazuhiro ^{[8
]}

Kiyota, Seiichiro ^{[9
]}

Tanabe, Kenji ^{[10
]}

Imamura, Kazuyoshi ^{[10
]}

Kunitomi, Nanae ^{[10
]}

Kunihiro, Kenji ^{[10
]}

Taguchi, Hiroki ^{[10
]}

Koizumi, Mitsuo ^{[10
]}

Yamada, Norimi ^{[10
]}

Nishi, Yuichi ^{[10
]}

Kida, Mayumi ^{[10
]}

Tanaka, Sawa ^{[10
]}

Ueoka, Rie ^{[10
]}

Yasui, Hideki ^{[10
]}

Maruoka, Koichi ^{[10
]}

Henden, Arne ^{[11
]}

Oksanen, Arto ^{[12
]}

Moilanen, Marko ^{[12
]}

Tikkanen, Petri ^{[12
]}

Mika, A.H.O. ^{[12
]}

Monard, Berto ^{[13
]}

Itoh, Hiroshi ^{[14
]}

Dubovsky, Pavol A. ^{[15
]}

Kudzej, Igor ^{[15
]}

Dancikova, Radka ^{[16
]}

Vanmunster, Tonny ^{[17
]}

Pietz, Jochen ^{[18
]}

Bolt, Greg ^{[19
]}

Boyd, David ^{[20
]}

Nelson, Peter ^{[21
]}

Krajci, Thomas ^{[22
]}

Cook, Lewis M. ^{[23
]}

机构：

[1] Department of Astronomy, Kyoto University, Sakyo-ku, Kyoto 606-8502, Kitashirakawa-Oiwake-cho

[2] Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, Kamogata, Asakuchi, Okayama 719-0232

[3] Astrophysical Science Center, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526

[4] Kwasan and Hida Observatories, Kyoto University, Yamashina-ku

[5] Subaru Telescope, National Astronomical Observatory of Japan, Hilo, HI 96720

[6] Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 229-8510

[7] Osaka Kyoiku University, Kashiwara, Osaka 582-8582

[8] Variable Star Observers League in Japan (VSOLJ), Isato-cho, Kumano, Mie 519-4673

[9] VSOLJ, Tsukuba, Ibaraki 305-0035

[10] Department of Biosphere-Geosphere System Science, Faculty of Informatics, Okayama University of Science, Okayama, Okayama 700-0005

[11] American Association of Variable Star Observers (AAVSO), Cambridge, MA 02138

[12] Nyrola Observatory, Jyvaskylan Sirius ry, FI-40270 Palokka

[13] Bronberg Observatory, Center for Backyard Astrophysics (Pretoria), Tiegerpoort 0056

[14] VSOLJ, Hachioji, Tokyo 192-0153

[15] Vihorlat Observatory, Humenne

[16] Phillips Academy Andover, Andover, MA 01810

[17] Center for Backyard Astrophysics (Belgium), B-3401, Landen

[18] 65510 Idstein

[19] Craigie, WA 6025, Camberwarra Drive

[20] West Challow, Wantage, OX12 9TX, Silver Lane

[21] RMB 2493

[22] Center for Backyard Astrophysics (New Mexico), Cloudcroft, NM 83117

[23] Center for Backyard Astrophysics (Concord), Concord, CA 94518

[24] Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka 560-0043

[25] DeKalb Observatory, H63, Auburn, IN 46706

[26] Pemberton, School Lane, Bunbury, Tarporley, Cheshire

[27] DK-8350 Hundslund

[28] Virtual Telescope Project, 03023 Ceccano, FR

[29] Project Eridanus, Observatory and Planetarium of Johann Palisa, VSB - Technical University Ostrava, Ostrava - Poruba 708 33

[30] Institute of Computer Science, Faculty of Civil Engineering, Brno University of Technology

[31] Center for Backyard Astrophysics (Flanders), American Association of Variable Star Observers (AAVSO), Alan Guth Observatory, Hofstade, Aalst

[32] Furzehill House, Ilston, Swansea

[33] VSOLJ, Juni-jo Minami, Nayoro, Hokkaido 096-0022

[34] American Association of Variable Star Observers (AAVSO), 5170 Lesve (Profondeville)

[35] Seikei Meteorological Observatory, Seikei High School, Musashino, Tokyo 180-8633

[36] Arch Cape Observatory, Arch Cape, OR 97102

[37] Hudson, NH 03051

[38] Southern Stars Observatory, 98702 FAAA Tahiti

[39] Woodridge Observatory, Eltham, VIC 3095

[40] Center for Backyard Astrophysics (Alberta), King's University College, Edmonton

[41] Conder Brow Observatory, Fell Acre, Conder Brow, Scotforth, Lancashire, LA2 ORQ, Little Fell Lane

[42] Physics Department, Rochester Institute of Technology, Rochester

[43] 59553 Lauwin Planque

[44] Crimean Astrophysical Observatory, 98409, Nauchny, Crimea

[45] Institute of Astronomy, Russian Academy of Sciences, 361605 Peak Terskol, Kabardino-Balkaria

[46] Department of Astronomy, University of Minnesota, Minneapolis, MN 55455

[47] Calgary, AB T2L 0X7

[48] Šíd Astronomical Observatory, Šíd 303

[49] Green Island Observatory, Geçitkale, Magosa, via Mersin

[50] Barfold Observatory, Glenhope, VIC 3444

来源：

Publications of the Astronomical Society of Japan | 2009年 / 61卷 / SPEC. ISS. 2期

关键词：

Accretion; accretion disks; Stars: dwarf novae; Stars:; novae; cataclysmic variables;

D O I：

10.1093/pasj/61.sp2.s395

中图分类号：

学科分类号：

摘要：

We systematically surveyed period variations of superhumps in SU UMa-type dwarf novae based on newly obtained data and past publications. In many systems, the evolution of the superhump period is found to be composed of three distinct stages: an early evolutionary stage with a longer superhump period, a middle stage with systematically varying periods, and a final stage with a shorter, stable superhump period. During the middle stage, many systems with superhump periods of less than 0.08 d show positive period derivatives. We present observational characteristics of these stages and give greatly improved statistics. Contrary to an earlier claim, we found no clear evidence for a variation of period derivatives among different superoutbursts of the same object. We present an interpretation that the lengthening of the superhump period is a result of the outward propagation of an eccentricity wave, which is limited by the radius near the tidal truncation. We interpret that late-stage superhumps are rejuvenated excitation of a 3:1 resonance when superhumps in the outer disk are effectively quenched. The general behavior of the period variation, particularly in systems with short orbital periods, appears to follow a scenario proposed in Kato, Maehara, and Monard (2008, PASJ, 60, L23). We also present an observational summary of WZ Sge-type dwarf novae. Many of them have shown long-enduring superhumps during a post-superoutburst stage having longer periods than those during the main superoutburst. The period derivatives in WZ Sge-type dwarf novae are found to be strongly correlated with the fractional superhump excess, or consequently with the mass ratio. WZ Sge-type dwarf novae with a long-lasting rebrightening or with multiple rebrightenings tend to have smaller period derivatives, and are excellent candidates for those systems around or after the period minimum of evolution of cataclysmic variables. © 2009. Astronomical Society of Japan.

引用

页码：S395 / S616

页数：221

共 362 条

[1] Alksnis A., Zacs L., IBVS, (1981)
[2] Altizer R., IAU Circ, (1972)
[3] Antipin S.V., IBVS, (1998)
[4] Antipin S.V., IBVS, (1999)
[5] Antipin S.V., Pavlenko E.P., A&A, 391, (2002)
[6] Antipin S.V., Samus N.N., Kroll P., IBVS, (2004)
[7] Araujo-Betancor S., Et al., A&A, 430, (2005)
[8] Argyle R.W., IAU Circ, (1983)
[9] Aungwerojwit A., Et al., A&A, 455, (2006)
[10] Baade W., Astron. Nachr, 232, (1928)

← 1 2 3 4 5 6 7 8 9 10 →