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20 April 2024 |
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The 2001 Superoutburst of WZ Sagittae | | J. Patterson
; G. Masi
; M. Richmond
; B. Martin
; E. Beshore
; D. Skillman
; J. Kemp
; T. Vanmunster
; R. Rea
; W. Allen
; S. Davis
; T. Davis
; A. Henden
; D. Starkey
; J. Foote
; A. Oksanen
; L. Cook
; R. Fried
; D. Husar
; R. Novak
; T. Campbell
; J. Robertson
; T. Krajci
; E. Pavlenko
; N. Mirabal
; P. Niarchos
; O. Brettman
; S. Walker ( CU
; CBA
; RIT
; KUC
; JAC
; USNO
; NCO
; ATU
; CAO
; | | Date: |
8 Apr 2002 | | Subject: | astro-ph | | Affiliation: | 5, 1), T. Vanmunster , R. Rea , W. Allen , S. Davis , T. Davis , A. Henden , D. Starkey , J. Foote , A. Oksanen , L. Cook , R. Fried , D. Husar , R. Novak , T. Campbell , J. Robertson , T. Krajci , E. Pavlenko , N. Mirabal , P. Niarchos (10), O. Brett | | Abstract: | We report the results of a worldwide campaign to observe WZ Sagittae during its 2001 superoutburst. After a 23-year slumber at V=15.5, the star rose within 2 days to a peak brightness of 8.2, and showed a main eruption lasting 25 days. The return to quiescence was punctuated by 12 small eruptions, of ~1 mag amplitude and 2 day recurrence time; these "echo outbursts" are of uncertain origin, but somewhat resemble the normal outbursts of dwarf novae. After 52 days, the star began a slow decline to quiescence. Periodic waves in the light curve closely followed the pattern seen in the 1978 superoutburst: a strong orbital signal dominated the first 12 days, followed by a powerful /common superhump/ at 0.05721(5) d, 0.92(8)% longer than P_orb. The latter endured for at least 90 days, although probably mutating into a "late" superhump with a slightly longer mean period [0.05736(5) d]. The superhump appeared to follow familiar rules for such phenomena in dwarf novae, with components given by linear combinations of two basic frequencies: the orbital frequency omega_o and an unseen low frequency Omega, believed to represent the accretion disk’s apsidal precession. Long time series reveal an intricate fine structure, with ~20 incommensurate frequencies. Essentially all components occurred at a frequency n(omega_o)-m(Omega), with m=1, ..., n. But during its first week, the common superhump showed primary components at n (omega_o)-Omega, for n=1, 2, 3, 4, 5, 6, 7, 8, 9 (i.e., m=1 consistently); a month later, the dominant power shifted to components with m=n-1. This may arise from a shift in the disk’s spiral-arm pattern, likely to be the underlying cause of superhumps. The great majority of frequency components ... . (etc., abstract continues) | | Source: | arXiv, astro-ph/0204126 | | Services: | Forum | Review | PDF | Favorites | |
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