In this paper we characterize the potentially dangerous asteroid 2023 DZ2, detected in the EURONEAR project, whose principal investigator is Dr. Marcel Popescu.
With our light curve and others, we calculate its rotation period at 6.2 minutes.
Etiqueta: photometry
(194513) 2001 XR2
Number: 194513
Designation: 2001 XR2
Name: –
First Date: 2018/07/31
Points: 421
P1: 6.826
P1 error: 0.001
Max. Ampl.: 0.51
Binary asteroid IAU announcement telegram
(4494) MARIMO
V. Benishek, Belgrade Astronomical Observatory; P. Pravec, H. Kucakova,
K. Hornoch, and P. Kusnirak, Ondrejov Observatory; A. Aznar, Isaac Aznar
Observatory, Alcublas, Valencia, Spain; A. Leroy, Association T60, Toulouse,
France; and R. Durkee, Shed of Science South Observatory, Pontotoc, TX, USA,
report that photometric observations taken with a 0.35-m telescope at the
Sopot Observatory in Serbia, a 0.65-m telescope at the Ondrejov Observatory,
a 0.35-m telescope at the Isaac Aznar Observatory, a 0.50-m telescope at Pic
du Midi Observatory, and a 0.50-m telescope at the Shed of Science South
Observatory during Jan. 14-Mar. 27 reveal that minor planet (4494) is a
binary system with an orbital period of 24.73 ± 0.02 hr. The primary
shows a period of 4.1209 ± 0.0002 hr and has a lightcurve amplitude of 0.12
magnitude at solar phases 0.4-10.5 degrees, suggesting a nearly spheroidal
shape. Mutual eclipse/occultation events that are 0.15 magnitude deep
indicate a lower limit on the secondary-to-primary mean-diameter ratio of
0.38. The mean absolute R magnitude in the Cousins system is H_R = 13.28
± 0.15, assuming the phase-relation slope parameter G = 0.24 ± 0.11.
2022 May 19 (CBET 5124) Daniel W. E. Green» [2022-05-20 07:32, Ondrejov]
(1717) Arlon
Number: 1717
Designation: –
Name: Arlon
First Date: 2016/03/28
Points: 129
P1: 5.149
P1 error: 0.004
Max. Ampl.: 0.09
Binary asteroid IAU announcement telegram
(2500) ALASCATTALO
V. Benishek, Belgrade Astronomical Observatory; P. Pravec, Ondrejov
Observatory; F. Pilcher, Organ Mesa Observatory, Las Cruces, NM, U.S.A.; A.
Marchini, R. Papini, and F. Salvaggio, Dipartimento di Scienze Fisiche, Della
Terra e Dell’Ambiente, University of Siena; J. Oey, Blue Mountains
Observatory, Leura, NSW, Australia; D. Pray, Sugarloaf Mountain Observatory,
South Deerfield, MA, U.S.A.; R. Durkee, Shed of Science South Observatory,
Pontotoc, TX, U.S.A.; W. Cooney, J. Gross, and D. Terrell, Sonoita Research
Observatory, Sonoita, AZ, U.S.A.; R. Goncalves, Linhaceira Observatory,
Tomar, Portugal; A. Aznar, Isaac Aznar Observatory, Alcublas, Valencia,
Spain; C. Odden, Phillips Academy, Andover, MA, U.S.A.; and J. Kemp,
Middlebury College, Middlebury, VT, U.S.A., report that photometric
observations taken with a 0.35-m telescope at the Sopot Observatory in Serbia,
a 0.35-m telescope at the Organ Mesa Observatory, a 0.30-m telescope at the
Astronomical Observatory of the University of Siena, a 0.35-m telescope at the
Blue Mountains Observatory, a 0.50-m telescope at the Sugarloaf Mountain
Observatory, a 0.50-m telescope at the Shed of Science South Observatory, a
0.50-m telescope at the Sonoita Research Observatory, a 0.35-m telescope at
the Linhaceira Observatory, a 0.35-m telescope at the Isaac Aznar Observatory,
and a 0.50-m telescope at the Mittelman Observatories at New Mexico Skies
during Mar. 20-May 19 reveal that minor planet (2500) is a binary system
with an orbital period of 169.1 ± 0.3 hr. The primary shows a period of
2.75123 ± 0.00009 hr and has a lightcurve amplitude of 0.19 magnitude at
solar phases 2-17 degrees, suggesting a nearly spheroidal shape. Mutual
eclipse/occultation events that are 0.15 to 0.27 magnitude deep indicate a
secondary-to-primary mean-diameter ratio of 0.39 ± 0.02.
2020 June 7 (CBET 4791) Daniel W. E. Green [2020-06-08 06:24, Ondrejov]
Binary asteroid IAU announcement telegram
(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.
(5037) Habing
Number: 5037
Designation: –
Name: Habing
First Date: 2020/02/23
Points: 244
P1: 2.8298
P1 error: 0.0004
Max. Ampl.: 0.25
(137199) 1999 KX4
Number: 153814
Designation: 2001 WN5
Name: –
First Date: 2019/11/18
Points: 104
P1: 4.65
P1 error: 0.01
Max. Ampl.: 0.28
The changing rotational lightcurve of Varuna and evidence for a close-in satelite
From CCD observations carried out with different telescopes, we present short-term photometric measurements of the large trans-Neptunian object Varuna in 10 epochs, spanning around 19 years.
We observe that the amplitude of the rotational light curve has changed considerably during this period of time from 0.41 to 0.55 mag… We propose that these changes in the rotational light-curve shape are due to a large and close-in satellite whose rotation induces the additional periodicity. The peak-to-valley amplitude of this oscillation is in the order of 0.04 mag. We estimate that the satellite orbits Varuna with a period of 11.9819 hr (or 23.9638 hr).
The Astrophysical Journal Letters, 883:L21 (7pp), 2019 September 20 © 2019. The American Astronomical Society.
Mainbelt asteroids lightcurve analysis from TAR telescope network: 2018 October- 2019 May
Lightcurves of twelve main-belt asteroids (MBA)
obtained with the Telescopio Robótico Abierto network
(TAR) and the Isaac Aznar Observatory from 2018
October to 2019 May are presented and analyzed to
derive the rotation period, lightcurve amplitude, and axis
size relationship.
http://aptog.com/wp-content/uploads/2019/12/2019MPBu___46__395A.pdf
(153814) 2001 WN5
Number: 153814
Designation: 2001 WN5
Name: –
First Date: 2019/11/18
Points: 104
P1: 4.65
P1 error: 0.01
Max. Ampl.: 0.28
(162082) 1998 HL1
Number: 162082
Designation: 1998 HL1
Name: –
First Date: 2019/11/25
Points: 485
P1: 11.00
P1 error: 0.2
Max. Ampl.: 0.27
2015 JD1
Number: –
Designation: 2015 JD1
Name: –
First Date: 2019/11/16
Points: 295
P1: 5.212
P1 error: 0.218
Max. Ampl.: 0.71
Binary asteroid IAU announcement telegram
(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
Binary asteroid discovery IAU announcement
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]