Open AccessPhotometric study of new southern SU UMa‐type dwarf novae and candidates: V877 Ara, KK Tel and PU CMa
Author(s) -
Kato Taichi,
Santallo Roland,
Bolt Greg,
Richards Tom,
Nelson Peter,
Monard Berto,
Uemura Makoto,
Kiyota Seiichiro,
Stubbings Rod,
Pearce Andrew,
Watanabe Tsutomu,
Schmeer Patrick,
Yamaoka Hitoshi
Publication year - 2003
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2003.06229.x
Subject(s) - physics , astrophysics , dwarf nova , stars , period (music) , orbital period , type (biology) , astronomy , white dwarf , biology , ecology , acoustics
We photometrically observed the three dwarf novae V877 Ara, KK Tel and PU CMa. We discovered the undisputed presence of superhumps in V877 Ara and KK Tel, with mean periods of 0.084 11(2) and 0.088 08(3) d, respectively. Both V877 Ara and KK Tel are confirmed to belong to long‐period SU UMa‐type dwarf novae. In V877 Ara, we found a large decrease of the superhump period . There is evidence that the period of KK Tel decreased at a similar or a more exceptional rate. Coupled with the past studies of superhump period changes, these findings suggest that a previously neglected diversity of phenomena is present in long‐period SU UMa‐type dwarf novae. The present discovery of a diversity in long‐period SU UMa‐type systems would become an additional step towards a full understanding of the dwarf nova phenomenon. PU CMa is shown to be an excellent candidate for an SU UMa‐type dwarf nova. We examined the outburst properties of these dwarf novae, and derived characteristic outburst recurrence times. Combined with the recently published measurement of the orbital period of PU CMa, we propose that PU CMa is the first object filling the gap between the extreme WZ Sge‐type and ER UMa‐type stars.