activity
19932018
most citedThe identification of the optical/IR counterpart of the 15.8-s transient X-ray pulsar XTE J1946+274

25 citations · 97 across the 12 of their papers we have counts for

collaborators

12 papers

astro-ph.SR2018★ 7 cited

Wind and nebula of the M33 variable GR290 (WR/LBV)

Olga Maryeva, Gloria Koenigsberger, Oleg Egorov +4

Context: GR290 (M33/V532=Romano's Star) is a suspected post-LBV star located in M33 galaxy that shows a rare Wolf-Rayet spectrum during its minimum light phase. In spite of many st…

astro-ph.SR2016★ 11 cited

GR 290 (Romano's Star): 2. Light history and evolutionary state

V. F. Polcaro, O. Maryeva, R. Nesci +11

We have built the historical light curve of the luminous variable GR 290 back to 1901, from old observations of the star found in several archival plates of M 33. These old recordi…

physics.hist-ph2013

Astronomical orientations in sanctuaries of Daunia

E. Antonello, V. F. Polcaro, A. M Tunzi Sisto +1

Prehistoric sanctuaries of Daunia date back several thousand years. During the Neolithic and Bronze Age the farmers in that region dug hypogea and holes whose characteristics sugge…

physics.hist-ph2013

Prehistoric sanctuaries in Daunia

E. Antonello, V. F. Polcaro, A. M. Tunzi +1

Daunia is a region in northern Apulia with many interesting archaeological sites, particularly of the Neolithic and Bronze Age. Beginning from the fifth millennium BC, the farmers…

astro-ph.SR2010

The Extreme LBV Star GR290 (Romano's Star) in M33. Optical Spectrophotometric Monitoring

V. F. Polcaro, R. F. Viotti, C. Rossi +3

We study the long term, S Dor-type variability and the present hot phase of the LBV star GR290 (Romano's Star) in M33 in order to investigate possible links between the LBV and WNL…

astro-ph.SR2009★ 20 cited

Toward Understanding The B[e] Phenomenon: III. Properties of the optical counterpart of IRAS 00470+6429

A. S. Miroshnichenko, E. L. Chentsov, V. G. Klochkova +19

FS CMa type stars are a group of Galactic objects with the B[e] phenomenon. They exhibit strong emission-line spectra and infrared excesses, which are most likely due to recently f…