A 60-night campaign on dwarf novae - I. Photometric variability of SU UMa and YZ Cnc | Zendy

J. van Paradijs | Zendy; P. A. Charles | Zendy; E. T. Harlaftis | Zendy; M. J. Arévalo | Zendy; J. E. F. Baruch | Zendy; P. J. Callanan | Zendy; J. Casares | Zendy; V. S. Dhillon | Zendy; Á. Giménez | Zendy; R. Gonzàlez | Zendy; I. G. Matinez-Pais | Zendy; D. H. P. Jones | Zendy; B. J. M. Hassall | Zendy; C. Hellier | Zendy; M. Kidger | Zendy; C. Lázaro | Zendy; T. R. Marsh | Zendy; K. O. Mason | Zendy; K. Mukai | Zendy; T. Naylor | Zendy; V. Reglero | Zendy; R. G. M. Rutten | Zendy; Robert Con Smith | Zendy

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A 60-night campaign on dwarf novae - I. Photometric variability of SU UMa and YZ Cnc

Author(s) -

J. van Paradijs,

P. A. Charles,

E. T. Harlaftis,

M. J. Arévalo,

J. E. F. Baruch,

P. J. Callanan,

J. Casares,

V. S. Dhillon,

Á. Giménez,

R. Gonzàlez,

I. G. Matinez-Pais,

D. H. P. Jones,

B. J. M. Hassall,

C. Hellier,

M. Kidger,

C. Lázaro,

T. R. Marsh,

K. O. Mason,

K. Mukai,

T. Naylor,

V. Reglero,

R. G. M. Rutten,

Robert Con Smith

Publication year - 1994

Publication title -

monthly notices of the royal astronomical society

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.058

H-Index - 383

eISSN - 1365-8711

pISSN - 0035-8711

DOI - 10.1093/mnras/267.3.465

Subject(s) - physics , light curve , dwarf nova , astrophysics , accretion disc , accretion (finance) , variation (astronomy) , cataclysmic variable star , astronomy , stars , white dwarf

A 60-night campaign on SU UMa, YZ Cnc and some secondary targets was carried out during 1988 December and 1989 January at the Observatorio del Roque de Los Muchachos (the 1988 International Time Project). The aim was to study the behaviour of these dwarf novae through their outburst cycle. Here we present the overall light curves of the main targets, SU UMa and YZ Cnc, which show that the optical fluxes continue to decrease after the end of the outburst. For YZ Cnc we find that, during quiescence, orbital variability is present, which may be interpreted as modulation caused by the bright-spot region. Near the end of an outburst, a weak, sinusoidal variation is observed; we discuss the possibility that this arises either from the secondary star or the accretion disc

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