Observatorio del Teide, IAC
In the main belt of asteroids, there exist pairs of asteroids that are on highly similar heliocentric orbits. They were discovered by Vokrouhlický and Nesvorný (2008) who showed that the asteroid pairs cannot be random coincidences of unrelated asteroids from the local asteroid population, but most of them must be genetically related pairs.
Being motivated by the progress in our knowledge and understanding of asteroid pairs, we underwent a thorough photometric study of a sample of nearly 100 asteroid pairs.
IAU CBET 4634
B. Christmann, Soucieu-en-Jarrest, France; P. Pravec, K. Hornoch, H.
Kucakova, and P. Kusnirak, Ondrejov Observatory; D. Pray, Sugarloaf Mountain
Observatory, South Deerfield, MA, U.S.A.; V. Benishek, Belgrade Astronomical
Observatory; R. Montaigut and A. Leroy, OPERA Observatory, France; A. Marchini,
R. Papini, and F. Salvaggio, Dipartimento di Scienze Fisiche, Della Terra e
Dell’Ambiente, University of Siena; A. Aznar Macias, Astronomia Para Todos
Observatories Group, Spain; and M. Serra-Ricart and J. Licandro, Instituto de
Astrofisica de Canarias, report that photometric observations obtained with a
0.20-m telescope at Soucieu-en-Jarrest, a 0.65-m telescope at Ondrejov
Observatory, a 0.50-m telescope at the Sugarloaf Mountain Observatory, a
0.35-m telescope at the Sopot Observatory in Serbia, a 0.20-m telescope at
the OPERA Observatory, a 0.30-m telescope at the Astronomical Observatory of
the University of Siena, and a 0.45-m telescope at Observatorio del Teide
during Feb. 17-Mar. 26 reveal that minor planet (1344) is a binary system
with an orbital period of 42.40 Â± 0.03 hr. The primary shows a period of
3.12219 Â± 0.00006 hr and has a lightcurve amplitude of 0.43 mag at solar
phases 5-9 deg. Mutual eclipse/occultation events that are 0.08 to 0.16
magnitude deep indicate a lower limit on the secondary-to-primary mean-
diameter ratio of 0.27. The mean absolute magnitude in the Cousins R
photometric system is H_R = 12.79 Â± 0.06, assuming the phase relation slope
parameter G = 0.24 Â± 0.11.
2019 June 3 (CBET 4634) Daniel W. E. Green» [2019-06-04 07:28, Ondrejov]
CCD photometric observations of the inner main-belt asteroid (20882) 2000 VH57 were made from 2018 Sept. 15 through Oct. 20. Analysis of the data showed that the asteroid is binary with a primary rotational period of 2.5586 hr and a satellite orbital period of 32.81 hr. Mutual eclipse/occultation events indicate a lower limit on the secondary-to-primary mean diameter ratio (Ds/Dp) of 0.23. During the period of observations, the primary and secondary lightcurves evolved as the viewing aspect changed. In particular, the depth of the secondary event increased significantly towards the end of the observations.
Nuestra entrevista en la revista Muy Interesante explicando la repercusión de este histórico hito.
Photometric observations of the near-Earth asteroid (31345) 1998 PG by Pravec et al. (2000) found a rotation period of 2.51620 h. Also found was a secondary period of 7.0035 h, or the double-period of 14.007 h, possibly indicating an additional body in the system.
An extended campaign by the authors in 2018 lead to a similar primary period of 2.5168 h. However, instead of a 7-hour secondary period, one of about 16 hours was found with the lightcurve showing apparent mutual events (occultations and/or eclipses).
Incluye una mesa redonda de ASTROTURISMO Y DESARROLLO LOCAL con la participación del sector turístico, la Administración Pública, aficionados a la Astronomía y empresas de organización de eventos astronómicos.
Modera: Amadeo Aznar, economista y astrónomo pro-am del Grupo de Observatorios Astronomía Para Todos. Gerente de Astronomía Para Todos.