Results are presented of a long-term spectroscopic and photometric monitoring of V 568 Cyg, a Be formerly indicated by Blaauw (1961) to be a runaway star, a classification not coinciding with that by Gies and Bolton (1986). Analysis of... more
Results are presented of a long-term spectroscopic and photometric monitoring of V 568 Cyg, a Be formerly indicated by Blaauw (1961) to be a runaway star, a classification not coinciding with that by Gies and Bolton (1986). Analysis of the strong fading around JD 2446641.6, reported by Blanco et al. (1987), seems to exclude the suggested eclipse scenario. This photometric
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... Richard J. Wainscoat PAST PRESIDENT Malcolm G. Smith ORGANIZING COMMITTEE Carlo Blanco, David L. Crawford, Margarita Metaxa, Woodruff T. Sullivan ... showed that the airports on the island of Hawaii are the major source of... more
... Richard J. Wainscoat PAST PRESIDENT Malcolm G. Smith ORGANIZING COMMITTEE Carlo Blanco, David L. Crawford, Margarita Metaxa, Woodruff T. Sullivan ... showed that the airports on the island of Hawaii are the major source of broad-spectrum light affecting Mauna Kea. ...
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Research Interests:
Rotational periods, V lightcurves, B-V color indexes, rotation axis direction and shape of five asteroids are presented. The B and V photoelectric observations were carried out at Serra la Nave stellar station of Catania Astrophysical... more
Rotational periods, V lightcurves, B-V color indexes, rotation axis direction and shape of five asteroids are presented. The B and V photoelectric observations were carried out at Serra la Nave stellar station of Catania Astrophysical Observatory during March and August 1992 and May, July and September 1993. The synodic rotational periods determined are: 121 Hermione (P = 9h.238±0h.010), 150 Nuwa (P = 8h.140±0h.005), 236 Honoria (P = 12h.333±0h.006), 287 Nephthys (P = 7h.580±0h.004), 377 Campania (P = 8h.48±0h.01). No variation of the (B-V) color with the rotation appears for the asteroids observed. The determination of the pole direction and shape is performed by applying the Amplitude-Magnitude method (Zappalà et al., Asteroids, Comets, Meteors, pp. 73–76. Uppsala Universitet, Reprocentralen, HSC, Uppsala, 1983) to the data collected by us and to those reported in the literature.