Number: 2343
Designation: –
Name: Siding Spring
First Date: 2015/11/16
Points: 134
P1: 2.101
P1 error: 0.003
Max. Ampl.: 0.17
(3523) ARINA
V. Benishek, Belgrade Astronomical Observatory; P. Pravec, Ondrejov
Observatory; M. Husarik, Skalnate Pleso Observatory; A. Marchini,
R. Papini, and F. Salvagio, Dipartimento di Scienze Fisiche, Della Terra
e Dell’Ambiente, University of Siena; W. Cooney, Starry Night
Observatory, Columbus, TX, U.S.A.; A. Aznar, Isaac Aznar Observatory,
Alcublas, Valencia, Spain; P. Santos-Sanz, A. Sota, F. J. Aceituno,
Instituto de Astrofísica de Andalucía-CSIC, Granada, Spain, R. Goncalves and R. Durkee, Shed of
Science South Observatory, Pontotoc, TX, U.S.A., report that photometric
observations taken with a 0.35-m telescope at the Sopot Observatory in
Serbia, a 0.61-m telescope at the Skalnate Pleso Observatory, a 0.30-m
telescope at the Astronomical Observatory of the University of Siena,
a 0.23-m telescope at the WBRO Florence Observatory, a 0.50-m telescope
at the Starry Night Observatory, a 0.90-m telescope at the Sierra Nevada
Observatory IAA-CSIC and a 0.50-m telescope at the Shed of
Science South Observatory during Mar. 2-May 16 reveal that minor planet
(3523) is a binary system with an orbital period of 29.26 +/- 0.02 hr.
The primary shows a period of 2.6742 +/- 0.0001 hr and has a lightcurve
amplitude of 0.08 magnitude at solar phases 9-13 degrees, suggesting a
nearly spheroidal shape. Mutual eclipse/occultation events that are
0.06 magnitude deep indicate a lower limit on the secondary-to-primary
mean-diameter ratio of 0.24.
(1480) AUNUS
V. Benishek, Belgrade Astronomical Observatory; P. Pravec, Ondrejov
Observatory; J. Oey, Blue Mountains Observatory, Leura, NSW, Australia;
R. Durkee, Shed of Science South Observatory, Pontotoc, TX, U.S.A.; C. Odden,
Phillips Academy, Andover, MA, U.S.A.; W. Cooney, Starry Night Observatory,
Columbus, TX, U.S.A.; J. Kemp, Middlebury College, Middlebury, VT, U.S.A.;
D. Pray, Sugarloaf Mountain Observatory, South Deerfield, MA, U.S.A.; J.
Gross and D. Terrell, Sonoita Research Observatory, Sonoita, AZ, U.S.A.; and
A. Aznar, Isaac Aznar Observatory, Alcublas, Valencia, Spain, report that
photometric observations taken with a 0.35-m telescope at the Sopot
Observatory in Serbia, a 0.35-m telescope at the Blue Mountains Observatory,
a 0.50-m telescope at the Shed of Science South Observatory, a 0.50-m
telescope at the Phillips Academy Observatory, a 0.50-m telescope at the
Starry Night Observatory, a 0.50-m telescope at the Mittelman Observatories
at New Mexico Skies, a 0.50-m telescope at the Sugarloaf Mountain
Observatory, a 0.50-m telescope at the Sonoita Research Observatory, and a
0.35-m telescope at the Isaac Aznar Observatory during Mar. 21-May 19 reveal
that minor planet (1480) is a binary system with an orbital period of 19.714
± 0.003 hr. The primary shows a period of 5.1600 ± 0.0002 hr and has a
lightcurve amplitude of 0.16 magnitude at solar phases 2-18 degrees,
suggesting a nearly spheroidal shape. Mutual eclipse/occultation events that
are 0.09 to 0.20 magnitude deep indicate a lower limit on the secondary-to-
primary mean-diameter ratio of 0.30.
(2019) VAN ALBADA
V. Benishek, Belgrade Astronomical Observatory; P. Pravec, Ondrejov
Observatory; R. Durkee, Shed of Science South Observatory, Pontotoc, TX,
U.S.A.; M. Husarik, M. Pikler, G, Cervak, and D. Tomko, Skalnate Pleso
Observatory; B. Christmann, Soucieu-en-Jarrest, France; A. Aznar, Isaac
Aznar Observatory, Alcublas, Valencia, Spain; D. Pray, Sugarloaf Mountain
Observatory, South Deerfield, MA, U.S.A.; F. Pilcher, Organ Mesa Observatory,
Las Cruces, NM, U.S.A.; V. Chiorny, Kharkiv Observatory; and A. Marchini, R..
Papini, and F. Salvaggio, Dipartimento di Scienze Fisiche, Della Terra e
Dell’Ambiente, University of Siena, report that photometric observations
taken with a 0.35-m telescope at the Sopot Observatory in Serbia, a 0.50-m
telescope at the Shed of Science South Observatory, a 0.61-m telescope at
the Skalnate Pleso Observatory, 0.28-m telescope at Soucieu-en-Jarrest, a
0.35-m telescope at the Isaac Aznar Observatory, a 0.50-m telescope at the
Sugarloaf Mountain Observatory, a 0.35-m telescope at the Organ Mesa
Observatory, a 0.70-m telescope at the Chuguev station of the Kharkiv
Observatory in Ukraine, and a 0.30-m telescope at the Astronomical
Observatory of the University of Siena during Sept. 22-Oct. 26 reveal that
minor planet (2019) is a binary system with an orbital period of 17.982 ±
0.003 hr. The primary shows a period of 2.7294 ± 0.0005 hr and has a
lightcurve amplitude of 0.16 magnitude at solar phases 2-3 degrees. Mutual
eclipse/occultation events that are 0.07 to 0.12 magnitude deep indicate a
lower limit on the secondary-to-primary mean-diameter ratio of 0.26.
2019 October 30 (CBET 4689) Daniel W. E. Green
(18303) 1980 PU
V. Benishek, Belgrade Astronomical Observatory; P. Pravec and P.
Kusnirak, Ondrejov Observatory; R. Durkee, Shed of Science South Observatory,
Pontotoc, TX, U.S.A.; D. Pray, Sugarloaf Mountain Observatory, South
Deerfield, MA, U.S.A.; V. Chiorny and O. Mikhalchenko, Kharkiv Observatory;
M. Husarik and M. Pikler, Skalnate Pleso Observatory; J. Oey, Blue Mountains
Observatory, Leura, NSW, Australia; P. Bacci and M. Maestripieri,
Astronomical Observatory, San Marcello Pistoiese, Italy; and A. Aznar, Isaac
Aznar Observatory, Alcublas, Valencia, Spain, report that photometric
observations taken with a 0.35-m telescope at the Sopot Observatory in
Serbia, a 0.50-m telescope at the Shed of Science South Observatory, a
0.50-m telescope at the Sugarloaf Mountain Observatory, a 0.70-m telescope
at the Chuguev station of the Kharkiv Observatory in Ukraine, a 0.61-m
telescope at the Skalnate Pleso Observatory, a 0.35-m telescope at the Blue
Mountains Observatory, a 0.60-m telescope at the San Marcello Pistoiese
Observatory, and a 0.35-m telescope at the Isaac Aznar Observatory during
Aug. 10-Oct. 2 reveal that minor planet (18303) is a binary system with an
orbital period of 12.270 ± 0.003 hr. The primary shows a period of
2.72627 ± 0.00010 hr and has a lightcurve amplitude of 0.10 magnitude at
solar phases 4-14 degrees, suggesting a nearly spheroidal shape. Mutual
eclipse/occultation events that are 0.05 to 0.12 magnitude deep indicate
a secondary-to-primary mean-diameter ratio of 0.24 ± 0.03.
2019 October 9 (CBET 4676) Daniel W. E. Green» [2019-10-10 07:45, Ondrejov]
IAU CBET 4634
(1344) CAUBETA
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 ± 0.03 hr. The primary shows a period of
3.12219 ± 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 ± 0.06, assuming the phase relation slope
parameter G = 0.24 ± 0.11.
2019 June 3 (CBET 4634) Daniel W. E. Green» [2019-06-04 07:28, Ondrejov]
http://aptog.com/wp-content/uploads/2019/04/2019MPBu___46__164W.pdf
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.
(31345) 1998 PG: A BINARY NEAR-EARTH ASTEROID?
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).