J/MNRAS/525/4581 NEA (23187) 2000 PN9 lightcurves (Dover+, 2023)
Physical modelling of near-Earth asteroid (23187) 2000 PN9 with ground-based
optical and radar observations.
Dover L., Lowry S.C., Rozek A., Rozitis B., Jackson S.L., Zegmott T.,
Krugly Yu.N., Belskaya I.N., Fitzsimmons A., Green S.F., Snodgrass C.,
Weissman P.R., Brozovic M, Benner L.A.M., Busch M.W., Ayvazian V.R.,
Chiorny V., Inasaridze R.Ya., Krugov M., Mykhailova S., Reva I., Hibbert J.
<Mon. Not. R. Astron. Soc. 525, 4581-4595 (2023)>
=2023MNRAS.525.4581D 2023MNRAS.525.4581D (SIMBAD/NED BibCode)
ADC_Keywords: Solar system ; Minor planets ; Photometry ; Optical
Keywords: radiation mechanisms: thermal - methods: data analysis -
methods: observational - techniques: photometric -
techniques: radar astronomy -
minor planets, asteroids: individual: (23187) 2000 PN9
Abstract:
We present a physical model and spin-state analysis of the potential
ly hazardous asteroid (23187) 2000 PN9. As part of a long-term
campaign to make direct detections of the YORP effect, we collected
optical lightcurves of the asteroid between 2006 and 2020. These
observations were combined with planetary radar data to develop a
detailed shape model which was used to search for YORP acceleration.
We report that 2000 PN9 is a relatively large top-shaped body with a
sidereal rotation period of 2.53216±0.00015h. Although we find no
evidence for rotational acceleration, YORP torques smaller than
∼10-8rad/day2 cannot be ruled out. It is likely that 2000 PN9
is a YORP-evolved object, and may be an example of YORP equilibrium or
self limitation.
Description:
Between 2006 and 2020 we conducted optical observations of (23187)
2000 PN9 from eight different observatories to obtain rotational
lightcurves.
Observations with the NTT with EFOSC2 were taken in 2010 and 2020,
under ESO programmes 185.C-1033 and 106.C-0794 respectively. We
conducted observations with the INT in 2020 under the programme
I/2020B/05. We observed the asteroid in 2010 with the 1.54 m Danish
Telescope, with observations carried out through the MiNDSTEp
consortium.
Further observations were conducted with Chuhuiv Observatory (2011),
Table Mountain Observatory (2010), Abastumani Observatory (2011), the
Hale Telescope (2015), Tien-Shan Observaotry (2015) and the Shain
Telescope (2015).
Also included are previously published lightcurve data from Chuhuiv
observatory in 2006 (see Belskaya et al. (2009)). Processed
lightcurves taken at Palmer Divide Observatory in 2016, which were
retrieved from the Asteroid Lightcurve Data Exchange Format (ALCDEF)
database, are included.
objects:
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Planet Name H i e a
mag deg AU
--------------------------------------------------------------
23187 2000PN9 15.9 51.3277716 0.5892360 1.8470312
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 66 35 All optical light curves of 2000 PN9 are
considered in this study
23187_lc.dat 40 1570 Optical lightcurves of NEA (23187) 2000 PN9
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- ID [1/35] Light curve number
4- 13 A10 "date" Obs.date UT date at the beginning of the nigh
15- 19 F5.3 AU Rsun Heliocentric distance
21- 25 F5.3 AU Rgeo Geocentric distance
27- 32 F6.2 deg alpha Solar phase angle
34- 38 F5.1 deg lambda0 Observed ecliptic longitude
40- 45 F6.2 deg beta0 Observed ecliptic latitude
47- 49 F3.1 h Total Total time over which the target was observed
51- 54 A4 --- Obs Facility observing facility (1)
56- 60 A5 --- Filter [BVRI clear] Photometric filter
62 A1 --- Incmod [*] * indicate which light curves were
included in the modelling
64 A1 --- Incpho [*] * indicate which light curves that were
included in the phase offset analysis
66 I1 --- Ref [1/2]? Reference (2)
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Note (1): Observing facility as follows:
ChO = Chuhuiv Observatory 0.7-m Telescope (121 - Kharkiv, Ukraine)
ESOD = European Southern Observatory Danish 1.54-m Telescope
(809 - La Silla, Chile)
NTT = European Southern Observatory 3.6-m New Technology Telescope
(809 - La Silla, Chile)
TMO = Table Mountain Observatory 0.6-m Telescope (673 - California, USA)
AbAO = Abastumani Astrophysical Observatory 0.7-m Telescope
(119 - Abastumani, Georgia)
TSAO = Tien-Shan Astronomical Observatory 1.0-m Telescope
(N42 - Almaty, Kazakhstan)
CrAO = Crimean Astrophyscial Observatory 2.6-m Shain Telescope
(095 - Nauchny, Ukraine)
PAL = Palomar Observatory 5.1-m Hale Telescope (675 - California, USA)
PDS = Palmer Divide Station 0.35m (various) (U82 - California, USA)
INT = Isaac Newton Group 2.54-m Isaac Newton Telescope
(950 - La Palma, Spain)
Note (2): References as follows:
1 = Belskaya et al. (2009, Icarus, 201, 167)
2 = Warner (Minor Planet Bulletin, , 43, 240)
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Byte-by-byte Description of file: 23187_lc.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.5 d JD Julian date at mid-point of exposure
(not light-time corrected)
15- 20 F6.3 mag mag Relative magnitude
22- 27 F6.4 mag e_mag 1-sigma uncertainty in relative magnitude
29- 33 A5 --- Filter [BVRI clear] Photometric filter
35- 37 A3 --- Obs Observatory used to obtain lightcurve (IAU code)
39- 40 I2 --- ID [1/35] Lightcurve ID (1)
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Note (1): There are 35 lightcurves included in this file.
Each lightcurve has an associated ID, which corresponds to Table 1 in the
paper.
Note that some nights have multiple lightcurves from the same facility
on the same date.
See Belskaya et al. (2009, Icarus, 201, 167) for lightcurves 1-6 and
Warner et al. (2011, Minor Planet Bulletin, 38, 172) and
Warner (2016, Minor Planet Bulletin, 43, 240) for lightcurves 24-30.
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Acknowledgements:
Lord Dover, lrd27[at]kent.ac.uk or astro[at]lorddover.com
(End) Patricia Vannier [CDS] 12-Sep-2023