Optical observations of selected asteroids with measurable Yarkovsky effect
The results of the observations of 10 asteroids for 2009-2012 and their analysis are presented here. The asteroids were selected based on the available list of asteroids with relatively large deviations from the unperturbed semimajor axis of the orbit that can be caused by Yarkovsky effect. The obse...
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| Цитувати: | Optical observations of selected asteroids with measurable Yarkovsky effect / A.V. Pomazan, N.V. Maigurova // Advances in Astronomy and Space Physics. — 2013. — Т. 3., вип. 2. — С. 113-115. — Бібліогр.: 7 назв. — англ. |
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irk-123456789-1196452017-06-08T03:07:51Z Optical observations of selected asteroids with measurable Yarkovsky effect Pomazan, A.V. Maigurova, N.V. The results of the observations of 10 asteroids for 2009-2012 and their analysis are presented here. The asteroids were selected based on the available list of asteroids with relatively large deviations from the unperturbed semimajor axis of the orbit that can be caused by Yarkovsky effect. The observations were made at RTT-150 (NO TUBITAK, Turkey) and Mobitel (RI NAO, Ukraine). We have calculated the differences between the observed (O) and the calculated (C) positions, as well as the standard deviations (RMS) of the measurements. For the telescope RTT-150, the RMS is approximately 0.05ʺ in both coordinates, and for the telescope Mobitel, the RMS is less than 0.1ʺ. 2013 Article Optical observations of selected asteroids with measurable Yarkovsky effect / A.V. Pomazan, N.V. Maigurova // Advances in Astronomy and Space Physics. — 2013. — Т. 3., вип. 2. — С. 113-115. — Бібліогр.: 7 назв. — англ. 2227-1481 http://dspace.nbuv.gov.ua/handle/123456789/119645 en Advances in Astronomy and Space Physics Головна астрономічна обсерваторія НАН України |
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The results of the observations of 10 asteroids for 2009-2012 and their analysis are presented here. The asteroids were selected based on the available list of asteroids with relatively large deviations from the unperturbed semimajor axis of the orbit that can be caused by Yarkovsky effect. The observations were made at RTT-150 (NO TUBITAK, Turkey) and Mobitel (RI NAO, Ukraine). We have calculated the differences between the observed (O) and the calculated (C) positions, as well as the standard deviations (RMS) of the measurements. For the telescope RTT-150, the RMS is approximately 0.05ʺ in both coordinates, and for the telescope Mobitel, the RMS is less than 0.1ʺ. |
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Article |
| author |
Pomazan, A.V. Maigurova, N.V. |
| spellingShingle |
Pomazan, A.V. Maigurova, N.V. Optical observations of selected asteroids with measurable Yarkovsky effect Advances in Astronomy and Space Physics |
| author_facet |
Pomazan, A.V. Maigurova, N.V. |
| author_sort |
Pomazan, A.V. |
| title |
Optical observations of selected asteroids with measurable Yarkovsky effect |
| title_short |
Optical observations of selected asteroids with measurable Yarkovsky effect |
| title_full |
Optical observations of selected asteroids with measurable Yarkovsky effect |
| title_fullStr |
Optical observations of selected asteroids with measurable Yarkovsky effect |
| title_full_unstemmed |
Optical observations of selected asteroids with measurable Yarkovsky effect |
| title_sort |
optical observations of selected asteroids with measurable yarkovsky effect |
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Головна астрономічна обсерваторія НАН України |
| publishDate |
2013 |
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http://dspace.nbuv.gov.ua/handle/123456789/119645 |
| citation_txt |
Optical observations of selected asteroids with measurable Yarkovsky effect / A.V. Pomazan, N.V. Maigurova // Advances in Astronomy and Space Physics. — 2013. — Т. 3., вип. 2. — С. 113-115. — Бібліогр.: 7 назв. — англ. |
| series |
Advances in Astronomy and Space Physics |
| work_keys_str_mv |
AT pomazanav opticalobservationsofselectedasteroidswithmeasurableyarkovskyeffect AT maigurovanv opticalobservationsofselectedasteroidswithmeasurableyarkovskyeffect |
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2025-07-08T16:19:37Z |
| last_indexed |
2025-07-08T16:19:37Z |
| _version_ |
1837096322769879040 |
| fulltext |
Optical observations of selected asteroids
with measurable Yarkovsky e�ect
A. V. Pomazan∗, N.V.Maigurova
Advances in Astronomy and Space Physics, 3, 113-115 (2013)
© A.V.Pomazan, N.V.Maigurova, 2013
Research Institute `Nikolaev Astronomical Observatory', Observatorna 1, 54030, Mykolaiv, Ukraine
The results of the observations of 10 asteroids for 2009�2012 and their analysis are presented here. The asteroids
were selected based on the available list of asteroids with relatively large deviations from the unperturbed semi-
major axis of the orbit that can be caused by Yarkovsky e�ect. The observations were made at RTT-150 (NO
TUBITAK, Turkey) and Mobitel (RI NAO, Ukraine). We have calculated the di�erences between the observed (O)
and the calculated (C) positions, as well as the standard deviations (RMS) of the measurements. For the telescope
RTT-150, the RMS is approximately 0.05′′ in both coordinates, and for the telescope Mobitel, the RMS is less than
0.1′′.
Key words: astrometry, asteroids, accuracy position
introduction
In recent decades, interest in non-gravitational ef-
fects in the motion of the small Solar System bod-
ies, has been increasing. These e�ects, together with
gravitational forces and collisions, signi�cantly a�ect
the dynamic evolution of the orbits of small bodies
in the Solar System. The accumulation of a long
series of high-precision optical observations of aster-
oids, and the presence of radar observations, will re-
veal such small e�ects.
The Yarkovsky e�ect is one of the most powerful
non-gravitational e�ects. This e�ect causes the shift
of the semi-major axis a of the orbit of an asteroid,
which could cause asteroids to drift from the main
belt to near-Earth space [1, 2]. Depending on the
direction of rotation of the asteroid, the Yarkovsky
e�ect can either increase or decrease the semi-major
axis of the orbit. When rotation is prograde, the jet
force from the thermal re-emission of absorbed solar
radiation is tangential to the direction of the asteroid
revolution, which causes a lengthening of the semi-
major axis (da/dt > 0). For retrograde rotation of an
asteroid, the force direction is opposite to the direc-
tion of its velocity revolution, which causes a short-
ening of the semi-major axis (da/dt < 0) [1, 5]. In
the papers [6, 7], it is shown that for an accurate cal-
culation of the orbital position, the Yarkovsky e�ect
must be taken into account when constructing mo-
tion models of small asteroids, along with the grav-
itational perturbations of the planets, their moons,
large asteroids, and several relativistic e�ects.
This e�ect has the most signi�cant a�ect on the
dynamic evolution of irregularly shaped kilometre-
sized asteroids. According to [5], an estimated value
of the semi-major axis drift for such asteroids caused
by the Yarkovsky e�ect, is ∼ 10−3 a.u./My. Such as-
teroids typically have faint magnitude, however mod-
ern precision radar and even optical observations,
which have accuracy better than 0.1′′, enable the de-
tection of small di�erences between the actual po-
sition of the asteroid and the calculated position,
purely from the gravitational model of motion, even
at short time intervals (i. e. several decades).
observational program
and instruments
The list of 94 asteroids given in [3] was used to
create an observation plan. Objects for observation
were chosen based on the technical characteristics of
the telescope and the presence of a well-documented
observational history of objects. Table 1 shows the
characteristics of asteroids which are included in the
plan of observations (data taken from the HORIZONS
system1).
From the Table 1 we can see that the semi-major
axis of an asteroid's orbit is determined with a preci-
sion of the order of 10−9 a.u., which allows us to dis-
tinguish drifts da/dt on the order of 10−8 a.u., caused
by the Yarkovsky e�ect for a ten-year observational
period.
The observations of asteroids were carried out at
two telescopes: the telescope Mobitel (RI NAO) and
the Russian-Turkish telescope RTT-150 (Turkey).
The telescope Mobitel (D = 0.5m, F = 3.0m)
is equipped with the CCD camera Alta U9000
∗anton@mao.nikolaev.ua
1http://ssd.jpl.nasa.gov/
113
Advances in Astronomy and Space Physics A.V. Pomazan, N.V.Maigurova
(3056×3056, 12×12mkm2) of Apogee Imaging Sys-
tems, which allows us to obtain imaging with a
42′ × 42′ �eld of view, with 0.83′′/pix scale. That
system enables us to obtain a su�cient number of
reference stars for reduction in the UCAC catalogues.
The observations were made in R Johnson-Cousins-
Bessel band.
The Russian-Turkish telescope RTT-150
(Turkey) (D = 1.5m, F = 11.6m) is equipped
with the modern CCD camera Andor DW436
(2048×2048, 13.5×13.5mkm2), which enables to ob-
tain imaging with a 8′ × 8′ �eld of view and scale of
0.24′′/pix. The telescope is equipped with a set of
UBV RI standard �lters of Johnson-Cousins-Bessel
band, which enables to conduct observations in mul-
tiple colour bands during one night [4].
the observations and analysis
of measuring observations
of asteroids
The 120 positions for 5 selected asteroids, from
the observations of 2011, were measured at the Mo-
bitel telescope. The equatorial coordinates of the as-
teroids at the epoch of observation were obtained as
result of standard astrometric reductions. We have
used the UCAC4 as the reference astrometric cata-
logue for reduction.
We have made the comparison of observed posi-
tions (O) with the calculated ephemeris (C) provided
by on-line service HORIZONS of the Jet Propulsion
Laboratory, USA2 and have calculated the residu-
als (O − C) in both coordinates, which are listed in
Table 2.
The Table 2 contains the date of observation, the
number of frames, magnitude of the object, (O−C)
di�erences and their standard errors (RMS) in both
coordinates. The mean internal accuracy of a sin-
gle position is 0.07′′ in right ascension and 0.08′′ in
declination for objects 9�16.5m. It was calculated
using standard deviations (O − C) in positions for
each series of observations.
Since 2004, regular observations of selected aster-
oids were carried out with telescope RTT-150 in var-
ious international projects. Images of objects listed
in [3], were selected from the available array of ob-
servations. The observations were reprocessed using
the catalogue UCAC4 as reference. Results of the
astrometric processing are presented in Table 3. The
mean internal accuracy of a single position is ap-
proximately 0.056′′ in right ascension and 0.042′′ in
declination for objects 14�19m.
conclusions
The use of high-precision CCD techniques has
made it possible to obtain accurate positions of small
asteroids, the size of which does not exceed several
kilometres, even using telescopes with a mirror diam-
eter of less than 1 meter. High positional accuracy of
the observational data suggests that these observa-
tions, together with other observations from Minor
Planet Centre (MPC), can be used to identify and
determine the value of the Yarkovsky e�ect.
references
[1] BottkeW.F., Jr., VokrouhlickýD., RubincamD.P. &
BrozM. 2002, in Asteroids III, eds.: BottkeW.F., Jr.,
CellinoA., Paolicchi P. & Binzel R. P., University of Ari-
zona Press, Tucson, 395
[2] Bro�zM., VokrouhlickýD., BottkeW.F. et al. 2006, IAU
Symposium 229, 351
[3] ChernetenkoYu.A. 2010, in Protecting the Earth against
Collisions with Asteroids and Comet Nuclei, Proc. of the
International Conf. �Asteroid-Comet Hazard 2009�, eds:
FinkelsteinA.M., HuebnerW.F. & ShorV.A., Nauka, St.
Petersburg, 289
[4] IvantsovA., PomazanA., KryuchkovskiyV. & GudkovaL.
2012, Odessa Astronomical Publications, 25, 66
[5] NugentC.R., Margot J. L., Chesley S.R. & Vokrouh-
lickýD. 2012, AJ, 144, 60
[6] VokrouhlickýD. 2006, A&A, 459, 275
[7] VokrouhlickýD., Chesley S.R. & MilaniA. 2001, Celestial
Mechanics and Dynamical Astronomy, 81, 149
Table 1: Characteristics of selected asteroids.
diameter, a, a-sigma, H Revolution Observation
Number km a.u. 10−9 a.u. e (mag) N period, year interval
1036 31.6 2.66 2.49 0.54 15.9 3423 4.34 1924�2013
1866 8.48 1.89 1.84 0.54 16.6 2194 2.61 1955�2013
1917 5.7 2.15 2.99 0.50 19.2 1082 3.15 1954�2013
1943 2.3 1.43 1.12 0.26 18.2 1649 1.71 1973�2012
2201 1.8 2.17 3.28 0.71 21.4 573 3.2 1931�2012
4179 5.4 2.53 0.15 0.63 20.3 5053 4.03 1934�2013
8567 3.1 2.05 10.68 0.45 19.8 2709 2.93 1955�2013
2http://ssd.jpl.nasa.gov/?horizons
114
Advances in Astronomy and Space Physics A.V. Pomazan, N.V.Maigurova
Table 2: The (O − C) di�erences and their standard errors for asteroids from observations at the telescope Mobitel.
H, (O − C), ′′ rms, ′′
Asteroid Date N (mag) RA Dec RA Dec
1036 2011-06-07 8 11.50 −0.032 −0.067 0.056 0.038
1036 2011-06-08 10 11.1 −0.045 −0.007 0.017 0.021
1036 2011-09-21 14 9.1 −0.043 0.13 0.036 0.02
1866 2011-06-07 9 14.2 −0.021 −0.005 0.1 0.083
1917 2011-06-06 5 16.3 −0.037 −0.136 0.06 0.026
1917 2011-06-08 10 16.7 −0.074 0.018 0.101 0.177
1917 2011-06-15 10 16.4 −0.035 0.04 0.069 0.099
1917 2011-06-16 3 16.4 0.029 −0.02 0.092 0.126
1917 2011-07-07 12 16.1 −0.088 −0.026 0.068 0.053
1917 2011-07-08 9 16.0 −0.105 −0.013 0.079 0.037
4179 2011-07-26 16 15.3 0.089 0.1 0.099 0.12
8567 2011-11-24 14 15.7 −0.251 0.144 0.068 0.174
mean 0.07 0.08
Table 3: The (O-C) di�erences and their standard errors for asteroids from observations at the telescope RTT-150.
H, (O-C), ′′ rms, ′′
Asteroid Date N (mag) RA Dec RA Dec
1943 2009-08-04 12 16.1 0.139 0.122 0.091 0.132
1943 2009-08-05 14 16.0 −0.015 0 0.061 0.006
1943 2009-08-06 14 16.2 −0.126 −0.03 0.049 0.017
1943 2009-08-07 12 16.1 0.017 −0.102 0.093 0.015
1943 2009-08-11 11 16.0 0.001 0.066 0.032 0.031
1943 2009-08-13 13 16.4 0.021 0.027 0.024 0.036
1943 2009-08-19 12 16.0 0.036 −0.024 0.016 0.015
2201 2009-08-11 6 18.9 0.05 −0.071 0.052 0.056
4179 2008-06-27 10 17.2 0.017 −0.03 0.036 0.055
4179 2008-06-30 7 17.2 −0.081 −0.042 0.078 0.073
4179 2008-07-03 7 17.5 −0.075 −0.017 0.08 0.026
4179 2008-12-02 32 14.1 −0.19 −0.026 0.06 0.038
mean 0.056 0.042
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