Apr-Jun, 31-2 - MinorPlanet.Info

29
THE MINOR PLANET
BULLETIN
BULLETIN OF THE MINOR PLANETS SECTION OF THE
ASSOCIATION OF LUNAR AND PLANETARY OBSERVERS
VOLUME 31, NUMBER 2, A.D. 2004 APRIL-JUNE
29.
CCD OBSERVATIONS AND PERIOD DETERMINATION
OF FIFTEEN MINOR PLANETS
photometric R (red) filter, although some observations required a
C (clear glass) filter for an improved signal-to-noise ratio.
Kevin Ivarsen
Sarah Willis
Laura Ingleby
Dan Matthews
Melanie Simet
In general we selected asteroids that did not have periods listed in
an October 2003 revision of the list of Harris (2003) and that
would be near opposition at the time of observation. At the
beginning of this project, eleven of the asteroids had undetermined
periods. However, by the project’s completion asteroids 1645
Waterfield and 228 Agathe were being studied by other
astronomers as posted on the CALL website
(http://www.minorplanetobserver.com/astlc/default.htm). Monson
(2004) presents a preliminary period determination for 1645
Waterfield that agrees with our data. No result for 228 had been
released at the time this paper was reviewed.
Department of Physics and Astronomy
Van Allen Hall
University of Iowa
Iowa City, IA 52242
kevin-ivarsen@uiowa.edu
(Received: 17 November
Revised: 15 February)
We have determined the periods of fifteen minor planets
using differential photometry. Eleven of these minor
planets had unknown periods, one had an uncertain
period, and three had well-known periods. We observed
a minimum of two epochs for each object in order to
construct composite lightcurves. The periods ranged
from 3.7 to 15.2 hours. The objects we report results for
are: 174 Phaedra, 228 Agathe, 342 Endymion, 354
Eleonora, 365 Corduba, 373 Melusina, 575 Renate,
1084 Tamariwa, 1171 Rusthawelia, 1388 Aphrodite,
1501 Baade, 1544 Vinterhanseni, 1645 Waterfield, 1799
Koussevitzky, and 2097 Galle.
We observed several minor planets from September 27 to October
21, 2003 using the Rigel Telescope (MPC Code 857; see
http://phobos.physics.uiowa.edu/tech/rigel.html) at the Winer
Observatory near Sonoita, Arizona (31° 39’ N 110° 37’ W). The
Rigel Telescope is a robotic facility operated remotely by faculty
and students at the University of Iowa for research and educational
use. We chose a site in Arizona because of the favorable seeing
conditions (2.5 to 3.5 arcsecond FWHM) and the number of clear
nights per year. The telescope is scheduled nightly and controlled
over the Internet.
The telescope is a 37 cm f/14 classical Cassegrain with a 16-bit
CCD camera. The camera is an FLI IMG-1024 with a backside
illuminated CCD sensor. In this telescope configuration the
camera has an image scale of 1 arcsecond per pixel. A signal to
noise estimate for 30-second exposures is shown in Figure 1.
Most of the images were taken using a Johnson-Cousins
To ensure the quality and accuracy of our experimental method,
we observed four asteroids with existing entries in the Harris list
and confirmed their periods. These asteroids are 174 Phaedra, 354
Eleonora, 575 Renate, and 1084 Tamariwa. Asteroid 1084
Tamariwa previously had two reported periods of 6.153 hours and
7.08 hours. Our initial period estimate matched the 7.08 hour
result, although this resulted in a very noisy combined lightcurve.
Further analysis revealed 6.19 hours as being a much better result.
We believe that the 7.08 hour period estimate can be discounted
with a high level of confidence.
Information about each epoch of observation is displayed in
Table I. Our results are summarized in Table II, and our
lightcurves are shown in the Appendix. Additional information
and data for all of our observations may be obtained from our
website, http://phobos.physics.uiowa.edu/research/asteroids. Our
results may also be found on the CALL website.
We thank Alan Harris for his careful review of the first draft of
this paper.
References
Harris, A. W. (2003). http://cfa-www.harvard.edu/iau/lists/Light
curveDat.html
Monson, A. (2004).
http://krypton.mnsu.edu/~monsoa1/welcome_files/Asteroid.htm
EDITOR’S NOTE: The team of Ivarsen et al. are to be
congratulated for their prolific results accomplished using a
robotic telescope at a distant favorable location. Their results
clearly demonstrate the highly productive capabilities of such
systems for asteroid lightcurve work.
Minor Planet Bulletin 31 (2004)
30
Table I – Observation details
Table II – Asteroid rotation results
Ast#
174
174
174
174
174
228
228
228
342
342
342
342
354
354
354
354
354
365
365
365
373
373
373
373
575
575
575
1084
1084
1084
1084
1171
1171
1388
1388
1388
1388
1388
1388
1501
1501
1501
1544
1544
1544
1544
1544
1645
1645
1799
1799
1799
1799
2097
2097
2097
2097
P.A.B.
Ast. Long. Lat. P.A. Range
174*
8 +10
4.0- 7.3
228
18
+4
3.8- 6.5
342
21
+5
2.8- 3.3
354* 352 -13
7.6-12.3
365
359
+1
2.3-11.1
373
0
0
2.5- 9.3
575* 359. +4
3.4- 4.4
1084*
20
-1
0.6- 1.7
1171
26
-4
1.9- 2.0
1388
7 -10
4.5- 8.1
1501
21
+1
0.6- 1.5
1544
9
-3
6.2- 9.3
1645
15
+1
3.4- 3.8
1799
9
-8
3.6- 7.4
2097
9
+5
2.8- 7.5
01
11
15
16
17
16
17
21
13
14
16
19
01
13
14
16
19
27
28
16
29
13
14
15
27
28
29
12
13
14
17
19
20
01
02
13
14
15
19
14
15
17
13
14
15
16
19
16
17
01
02
16
17
30
11
15
17
Epoch
Filter Exposure #Images Mag
Oct 03
R
15
84
13.0
Oct 03
R
30
38
12.8
Oct 03
R
30
49
12.8
Oct 03
R
30
38
12.5
Oct 03
R
30
54
12.5
Oct 03
R
30
39
13.5
Oct 03
R
30
60
13.4
Oct 03
R
30
38
13.6
Oct 03
R
30
62
12.6
Oct 03
R
30
62
12.5
Oct 03
R
15
27
12.8
Oct 03
R
30
58
12.8
Oct 03
R
30
37
11.0
Oct 03
R
30
38
11.5
Oct 03
R
30
35
11.4
Oct 03
R
15
14
11.5
Oct 03
R
30
32
11.7
Sep 03
C
15
133
12.8
Sep 03
R
30
56
12.3
Oct 03
R
30
42
12.6
Sep 03
R
15
68
13.6
Oct 03
R
15
23
14.0
Oct 03
R
15
16
13.6
Oct 03
R
15
44
13.9
Sep 03
C
15
131
13.7
Sep 03
R
30
54
13.8
Sep 03
R
30
69
14.1
Oct 03
R
15
10
14.1
Oct 03
R
15
10
13.9
Oct 03
R
15
43
13.5
Oct 03
R
15
67
14.1
Oct 03
R
15
84
13.4
Oct 03
R
15
41
13.0
Oct 03
R
15
36
15.3
Oct 03
R
30
31
15.4
Oct 03
R
30
44
15.4
Oct 03
R
30
47
15.6
Oct 03
R
15
34
15.8
Oct 03
R
30
45
16.0
Oct 03
R
15
47
13.7
Oct 03
R
15
49
13.9
Oct 03
R
15
73
14.0
Oct 03
R
30
55
15.2
Oct 03
R
30
53
15.0
Oct 03
R
15
35
15.0
Oct 03
R
15
29
15.3
Oct 03
R
30
53
15.6
Oct 03
R
30
59
14.2
Oct 03
C
20
100
14.4
Oct 03
R
15
64
15.4
Oct 03
R
20
47
15.3
Oct 03
R
30
38
15.7
Oct 03
C
20
45
15.6
Sep 03
R
30
98
14.6
Oct 03
R
30
50
15.5
Oct 03
R
30
50
15.4
Oct 03
R
30
55
15.2
Period (H)
5.75 ±0.001
6.47 ±0.01
7.05 ±0.01
4.277 ±0.001
6.354 ±0.001
12.97 ±0.01
3.678 ±0.001
6.19 ±0.01
10.98 ±0.01
11.95 ±0.01
15.25 ±0.01
13.7 ±0.1
4.876 ±0.01
6.325 ±0.001
7.310 ±0.005
Amp
0.52
0.30
0.18
0.15
0.20
0.23
0.18
0.25
0.36
0.50
0.33
0.28
0.23
0.37
0.45
* = Existing entry in Harris List as of Oct 2003
Figure 1. Signal to noise estimate for the Rigel telescope.
APPENDIX:
Composite lightcurves for 15 asteroids observed at the Winer
Observatory, September – October 2003.
Minor Planet Bulletin 31 (2004)
31
Minor Planet Bulletin 31 (2004)
32
Minor Planet Bulletin 31 (2004)
33
LIGHTCURVE PHOTOMETRY OF MARS-CROSSING
ASTEROIDS 1474 BEIRA AND 3674 ERBISBUHL
Robert A. Koff
980 Antelope Drive West
Bennett, CO 80102
bob.koff@worldnet.att.net
(Harris et al., 1989). This program allows compensation for nightto-night comparison star variation by manually shifting individual
night’s magnitude scales to obtain a best fit.
Observations and Results
1474 Beira
(Received: 2 January)
This is a report on the lightcurve measurement program
at Antelope Hills Observatory in the United States.
Asteroid 1474 Beira was determined to have a period of
4.184 hours ± 0.001 hours, with an amplitude of 0.18 ±
0.02 magnitude. Asteroid 3674 Erbisbuhl exhibited a
period of 11.28 hours ±0.01 hours and an amplitude of
0.40 ± 0.02 magnitude.
Equipment and Procedure
In 2002, Antelope Hills Observatory was established as a
replacement for Thornton Observatory, MPC code 713. The new
observatory is located near Bennett, Colorado at an elevation of
1740 meters. The observatory has obtained the MPC code H09.
The equipment and instrumentation of Antelope Hills Observatory
consists of an 0.25-m f/10 Meade SCT telescope, a True
Technology filter wheel, and an Apogee AP47 camera, operated
unbinned. The instruments are housed in a clamshell dome, and
are operated remotely from the nearby house. Targets were
selected from the “Potential Lightcurve Targets” on the CALL
website (Warner, 2003), and further refined based on their
magnitude and position in the sky. Targets were selected for which
no lightcurve data had been previously reported. (Harris, 1997).
Mars-crossing asteroids were given priority.
All images reported here were obtained in unfiltered light, using a
clear filter with an IR cutoff of 700 nm to prevent fringing. The
differential photometry was measured using the program
“Canopus” by Brian Warner, which uses aperture photometry.
Magnitudes were calculated using reference stars from the USNOA 2.0 catalog. Comparison stars differed from night-to-night due
to movement of the asteroid. Lightcurves were prepared using
“Canopus”, based on the method developed by Dr. Alan Harris
Beira, a Mars-crossing asteroid, was discovered August 20, 1935
by C. Jackson at Johannesburg, S. A. It is approximately 19 km
in diameter. The aphelion is 4.072 AU and the perihelion is
1.400 AU. No lightcurve results are reported for this object
(Harris 2004). Observations were made on six nights during the
period from September 2, 2003 to November 12, 2003. During
the period of the investigation, the phase angle dropped from 35.5
degrees to 34.0 degrees before increasing to 40.75 degrees.
Exposure times for this investigation were two minutes each.
Images were taken at 2.5-minute intervals. Dark frames and flat
fields were used to calibrate each image. A total of 463
observations were used in the solution.
Figure 1 shows the resulting lightcurve. The zero point of the
curve is J.D. 2452887.72249. The synodic period was determined
to be 4.184 hours with a formal error of ± 0.001 hours. The
amplitude was 0.18 ± 0.02 magnitude.
Figure 1. Lightcurve of 1474 Beira, based on a period of 4.184
hours. Ordinate is relative magnitude.
Minor Planet Bulletin 31 (2004)
34
3674 Erbisbuhl
Erbisbuhl is a Mars-crossing asteroid discovered September 13,
1963 by C. Hoffmeister at Sonneberg. It is approximately 25 km
in diameter. The aphelion is 3.243 AU, and perihelion is 1.479
AU. No previously observed lightcurve is reported for this object
(Harris 2004). Observations were made on three nights during the
period from December 17, 2003 to December 26, 2003. During
the period of the investigation, the phase angle dropped from 15.5
degrees to 11.0 degrees. Exposure times for this investigation
were two minutes each. Images were taken at 2.5-minute
intervals. Dark frames and flat fields were used to calibrate each
image. A total of 492 observations were used in the solution.
Figure 2 shows the resulting lightcurve. The zero point of the
curve is J.D. 2452990.75470. The synodic period was determined
to be 11.28 hours with a formal error of ± 0.01 hours. The
amplitude was 0.40 ± 0.02 magnitude. In addition to the clear
filter images used in the period solution, four images were taken
using V and R filters, and transformed to the standard system.
The resultant V-R for asteroid 3647 was 0.47 with an estimated
error of ±0.05.
LIGHTCURVE ANALYSIS OF ASTEROIDS
110, 196, 776, 804, AND 1825
Donald P. Pray
Carbuncle Hill Observatory
P.O. Box 946
Coventry, RI 02816
dppray@hotmail.com
(Received: 14 January
Revised: 10 February)
Lightcurve period and amplitude results are reported for
five asteroids observed at Carbuncle Hill Observatory
during November 2003 through January 2004. The
following synodic periods and amplitudes were
determined: 110 Lydia, 10.924+0.003h, 0.14+0.01m;
196 Philomela,
8.33+0.02h,
0 . 1 0+0.02m;
776 Berbericia, 7.67+0.04h, 0.26+0.01m; 804 Hispania,
14.64+0.01h, 0.20+0.02m; 1825 Klare, 4.744+0.009h,
0.75+0.02m
Introduction
Carbuncle Hill Observatory, MPC code 100, is located about
twenty miles west of Providence, RI, in one of the darkest spots in
the state. All observations were made using an SBIG ST-10XME
CCD camera, binned 3x3, coupled to a 0.35m f6.5 SCT. This
combination produced an image dimension of 21x14 arc min. All
observations were taken through the “clear” filter.
Figure 2. Lightcurve of 3674 Erbisbuhl, based on a period of
11.28 hours. Ordinate is relative magnitude.
Acknowledgments
Many thanks to Brian Warner for his continuing work on the
CALL website and the program “Canopus”, which has made it
possible for amateurs to analyze and share lightcurve data.
References
Harris, A. W., Young, J. W., Bowell, E., Martin, L. J., Millis, R.
L., Poutanen, M., Scaltriti, F., Zappala, V., Schober, H. J.,
Debehogne, H., and Zeigler, K. W. (1989). “Photoelectric
Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77, pp.
171-186.
Harris, A. W. (2004). “Minor Planet Lightcurve Parameters”, On
the Minor Planet Center website: http://cfa-www.harvard
.edu/iau/lists/LightcurveDat.html, or on the CALL website:
http://www.MinorPlanetObserver.com/astlc/default.htm
Warner, B. D. (2003). “Potential Lightcurve Targets”, on the
CALL website, http://www.MinorPlanetObserver.com/astlc/
default.htm
Most of the selected asteroids were observed as part of the
A.L.P.O. Shape Modeling Program. Details of this program may
be found at http://www.bitnik.com/mp/alpo/. The aim of the
program is to determine the pole position, shape, rotation state and
surface scattering properties of asteroids. Lightcurves generated
over several apparitions are generally required to make these
determinations. The four asteroids selected for this study already
had previously measured periods, so it is the differences between
the newly-found lightcurves and those which preceded them that is
significant. Targets were also selected based on their location
above the local horizon, as well as for their suitability to the
equipment. 1825 Klare was selected from the “Call” website’s
“List of Potential Lightcurve Targets” (Warner 2003). This target
did not have its period published in the list of “Minor Planet
Lightcurve Parameters” maintained by Harris and Warner (2003).
Image calibration via dark frames and flat field frames was
performed using “MaxIm DL”. Lightcurve construction and
analysis was accomplished using “Canopus” developed by Brian
Warner. Differential photometry was used in all cases, and all
measurements were corrected for light travel time.
Observations and Results
110 Lydia
Discovered by A. Borrelly at Marseille in 1870, 110 Lydia was
determined to have a synodic period of 10.924+0.003h, with an
amplitude of 0.14+0.01m. 597 images taken in ten sessions
between December 2 and December 29, 2003 were used to make
this measurement. The lightcurve is shown in Figure 1. This
period is compared to 10.927h, with an amplitude ranging between
0.10 and 0.20m, which is presented in the list of Minor Planet
Lightcurve Parameters, Harris and Warner (2003). The IRAS
Minor Planet Bulletin 31 (2004)
35
Minor Planet Survey, as appears in the Small Bodies Node of
NASA’s Planetary Data System, (henceforth IRAS V4.0), lists
110 Lydia as having an assumed absolute magnitude of 7.80, a
mean albedo of 0.181, and an effective diameter of 86 km.
maxima. If and when their shapes are determined, it should be
interesting to see what form they take. The list of Minor Planet
Lightcurve Parameters states this object as having a period of
7.668h with amplitude estimates between 0.13m and 0.21m. The
mean albedo is stated as 0.066 with an assumed absolute
magnitude of 7.68, yielding an effective diameter of 151 km,
(IRAS V4.0).
Figure 1. The lightcurve of 110 Lydia. The synodic period was
found to be 10.924+0.003h with an amplitude of 0.14+0.01m.
196 Philomela
C.H.F. Peters discovered this asteroid in 1879 at Clinton. IRAS
V4.0 has estimated a diameter of 136 km for this object with an
assumed absolute magnitude of 6.55. During three sessions
between November 16 and November 23, 2003, 559 images were
taken to derive a synodic period of 8.33+0.02h with an amplitude
of 0.10+0.02m. See Figure 2. During this time, the phase angle
changed from 8.6 to 6.3 degrees. The list of Minor Planet
Lightcurve Parameters lists this object as having a period of
8.343h, with various amplitudes between 0.07 and 0.37m.
Figure 3. The lightcurve for 776 Berbericia. The synodic period
was determined to be 7.67+0.04h with an amplitude of
0.26+0.01m.
804 Hispania
Hispania was discovered in 1915 at Barcelona by J. Comas Sola.
The mean albedo is listed as 0.052 with an assumed absolute
magnitude of 7.84, yielding an effective diameter of 157 km,
(IRAS V4.0). Ambiguity seems to have followed this object
throughout the years of effort to determine its rotational lightcurve
period. The list of Minor Planet Lightcurve Parameters shows a
period of 14.840h, and an amplitude between 0.19 and 0.23m.
However, examination of the references provided in the list show
other determinations have been made in the area of 7.4h,
Magnusson and Langerkvist (1991), Calabresi and Roselli (2001).
New lightcurve observations of Hispania were obtained from
December 9 to December 28, 2003, during which a total of 177
images were taken during four sessions. My initial analysis
showed a synodic period of 7.462+0.015h with an amplitude of
Figure 2. The lightcurve of 196 Philomela. The synodic period
was found to be 8.33+0.02h with an amplitude of 0.10+0.02m.
776 Berbericia
This object was discovered at Heidelburg by A. Massinger in
1914. The synodic period was determined to be 7.67+0.04h with
an amplitude of 0.26+0.01m. 386 images were taken in two
sessions over a three-night span between November 24 and
November 26, 2003. This asteroid is seen to have a somewhat
unusual lightcurve with four maxima, although one of these is
quite small. See Figure 3. Interestingly, it has roughly similar
features to the lightcurve of 110 Lydia, which also shows four
Figure 4. The lightcurve for 804 Hispania. The synodic period
was found to be 14.64+0.01h with an amplitude of 0.24+0.01m.
Minor Planet Bulletin 31 (2004)
36
0.20+0.02m. However, consultations with Robert Stevens of
Santana Observatory led me to revise the period upward to nearly
double this. Using his much larger data set as a guide for analysis,
I now derive a period of 14.64+0.01h with an amplitude of
0.24+0.01m. However, there is a rather large hole in the curve, so
these parameters could well change somewhat with better
coverage. The lightcurve is shown in Figure 4.
Acknowledgments
Special thanks is given to Brian Warner for his continued help and
support in my development in this area of research, and for his
continuing improvements to the program, “Canopus”. Thanks are
also given to Bob Stevens for his assistance with the solution of
the 804 Hispania lightcurve.
References
1825 Klare
This asteroid was discovered by K. Reinmuth at Heidelberg in
1954. 438 images were taken between December 27, 2003 and
January 1, 2004, in five sessions. The measured synodic period
was 4.744+0.009h with an amplitude of 0.75+0.02m. The large
amplitude would suggest a highly irregular shape. It was observed
at phase angles varying from 6 to 3.5 degrees. The lightcurve is
presented in Figure 5.
Calabresi, M., and Roselli, G. (2001). “Research Note, The
Rotation Period of 804 Hispania. Some Considerations on its
Nature.” Astronomy and Astrophysics, 369, 305-307.
Harris, Alan W., and Warner, Brian D. (2003). “Minor Planet
Lightcurve Parameters”, found on the Minor Planet Center web
site: http://cfa-www.harvard.edu/iau/lists/LightcurveDat.html.
IRAS V4.0 from NASA Small Bodies Node of the Planetary Data
System, IRAS Minor Planet Survey V4.0. http://pdssbn.astro
.umd.edu/nodehtml/sbdb.html
Magnusson, P., and Langerkvist, C. I. (1991). “Physical Studies
of Asteroids XXII. Photoelectric Photometry of Asteroids 34, 98,
115, 174, 270, 389, 419 and 804.” Astronomy and Astrophysics
Supplement Series 87, 269-275.
Stevens, R. (2004). Private communications.
.earthlink.net/~rdstephens/default.htm
http://home
Warner, B.D. (2003). Collaborative Asteroid Lightcurve Link
(CALL) web site. http://www.MinorPlanetObserver.com/astlc/
default.htm.
Figure 5. The lightcurve for 1825 Klare. The measured synodic
period was 4.744+0.009h with an amplitude of 0.75+0.02m.
LIGHTCURVE ANALYSIS FOR NUMBERED ASTEROIDS
1351, 1589, 2778, 5076, 5892, AND 6386
Brian D. Warner
Palmer Divide Observatory
17995 Bakers Farm Rd.
Colorado Springs, CO 80908
brian@MinorPlanetObserver.com
(Received: 6 January
Revised: 17 January)
The lightcurves of six numbered asteroids obtained in late
2003 were analyzed. The following synodic periods and
amplitudes were determined. 1351 Uzbekistania:
73.90±0.02h, 0.34±0.02m; 1589 Fanatica: 2.58±0.05h,
0.16±0.02m; 2778 Tangshan: 3.461±0.020h, 0.25±0.03m;
5076 Lebedev-Kumach: 3.2190±0.0005h, 0.14±0.02m;
(5892) 1981 YS1: 10.60±0.02h, 0.26±0.03m; and (6386)
1989 NK1: 3.1381±0.0005h, 0.08±0.02m.
Equipment and Procedures
The asteroid lightcurve program at the Palmer Divide Observatory
has been previously described in detail (Warner 2003) so only a
summary is provided now. The main instrument at the
Observatory is a 0.5m f/8.1 Ritchey-Chretien telescope using a
Finger Lakes Instruments IMG camera with Kodak KAF-1001E
chip. A second instrument also in use was a 0.3m f/9.3 SchmidtCassegrain using an SBIG ST-9E camera. For this set of asteroids,
only the 0.5m scope was used.
Initial targets are determined by referring to the list of lightcurves
maintained by Dr. Alan Harris (Harris 2003), with additions made
by the author to include findings posted in subsequent issues of
the Minor Planet Bulletin. In addition, reference is made to the
Collaborative Asteroid Lightcurve Link (CALL) web site
maintained by the author (http://www.MinorPlanetObserver
.com/astlc/default.htm) where researchers can post their findings
pending publication. MPO Canopus, a custom software package
written by the author, is used to measure the images. It uses
aperture photometry with derived magnitudes determined by
calibrating images against field or, preferably, standard stars. Raw
instrumental magnitudes are used for period analysis, which is
included in the program. The routine is a conversion of the
original FORTRAN code developed by Alan Harris (Harris et al.,
1989).
Note: in the following, the orbital elements are taken from the
IAU MPCORB data file available at the Minor Planet Center web
site (ftp://cfa-ftp.harvard.edu/pub/MPCORB/). The date of
osculation for the elements was 2453000.5.
Minor Planet Bulletin 31 (2004)
37
The Phase Angle Bisector
The observation table for each asteroid gives the date, phase angle,
and phase angle bisector longitude and latitude. The PAB was
developed by Alan Harris and Edward Bowell. Harris states
(Harris 2003a), “The significance is that the direction that bisects
the directions to the sun and the line of sight is a best
approximation to a single ‘viewing direction.’ As an extreme
example, if you viewed a rotating ‘cigar’ from its pole it would
have no lightcurve amplitude if the sun were also shining from the
pole direction, but if the sun were shining at the equator (90°
phase angle), then you would see a big amplitude. Now if you
reverse the Earth and sun positions so you are viewing from the
equator and the sun is shining on the pole, you likewise get a big
amplitude, even though in this case the illuminated area is
constant, you just see different amounts of it as it rotates. The best
approximation you can make to a zero phase angle viewing aspect
is a single line half way in between the illumination and viewing
directions. This we call the ‘phase angle bisector’, since it is the
line that bisects the phase angle.”
includes, among others, 48 Doris and 52 Europa. The IRAS
survey (Tedesco 1989) gives an effective diameter of 64.91 ±
4.31km and mean albedo of 0.0606 ±0.0090. The IAUs
MPCORB database gives values of 9.6 and 0.15 respectively for H
and G. The principal orbital elements for Uzbekistania are: semimajor axis, 3.197AU; inclination, 9.703°; and eccentricity, 0.0610.
There were 871 data points used in the final analysis that gave a
synodic period of 73.90±0.02h and amplitude of 0.34±0.02m.
Figure 1 shows the observations phased against this period. The
amplitude implies a ratio of 1.37:1 for the projected a/b axes of the
assumed triaxial ellipsoid. The table below provides a summary
of the individual observation runs.
1589 Fanatica
Results
M. Itzigsohn discovered 1589 Fanatica on 1950 September 13 at
La Plata. The name is in honor of Eva Peron whose devotion and
enthusiasm for the people of Argentina led her to champion the
cause of workers. The name literally means a fanatical woman or
feminine zealot. The asteroid has been designated 1935 RD, 1937
CF, 1946 OE, 1950 RK, 1950 TM3, and A924 WC.
Uzbekistania was discovered by G.N. Neujmin at Simeis on 1934
October 5. It’s carried the designations 1925 CA, 1928 QJ, 1931
FK, 1934 TF, A917 SL, and A920 FA. It’s named in honor of the
(former) Uzbek Soviet Republic where the discoverer lived during
WW II. Kozai (1979) puts the asteroid in his group 63, which
The H value from the MPCORB database 12.00. Using a formula
provide by Harris (2003), which assumes the asteroid’s albedo
(0.18) and type (S) based on the semi-major axis, the approximate
diameter is 12 km. Kosai (1979) includes Fanatica in his group 15
along with 11 Parthenope and 17 Thetis. The principal elements
are: semi-major axis, 2.417AU; inclination, 5.261°; and
eccentricity, 0.0927.
1351 Uzbekistania
Observations were obtained on three nights in late November and
early December, with a total of 261 data points used in the final
period analysis (see Figure 2). The synodic period was found to
be 2.58±0.05h and the amplitude to be 0.16±0.02m, or a projected
Figure 1. The lightcurve for 1351 Uzbekistania. The synodic
period is 73.9±0.02h and the amplitude 0.34±0.02m.
DATE
2003
Oct.
Oct.
Nov.
Nov.
Nov.
Nov.
Nov.
Nov.
Nov.
09
12
04
15
16
17
19
21
24
Phase
Angle
15.0
14.3
7.7
4.5
4.3
4.1
3.8
3.6
3.7
PAB
Long
58.2
58.5
59.4
59.4
59.4
59.4
59.4
59.4
59.4
Lat
7.5
7.6
8.6
9.0
9.0
9.1
9.1
9.2
9.3
Figure 2. The lightcurve for 1589 Fanatica phased against a
synodic period of 2.58±0.05h. The amplitude is 0.16±0.02m.
DATE
2003
Nov. 29
Nov. 30
Dec. 01
Minor Planet Bulletin 31 (2004)
Phase
Angle
7.9
8.4
8.9
PAB
Long
52.7
52.8
52.8
Lat
–4.1
–4.0
-4.0
38
a/b ratio of 1.16:1 for the assumed triaxial ellipsoid. The table
below provides a summary of the individual observation runs.
2778 Tangshan
amplitude to be 0.14±0.02m. Assuming a triaxial ellipsoid, the
amplitude gives a ratio of 1.14:1 for the projected a/b axes. Figure
4 shows a phased plot against this period. The table below
provides a summary of the individual observation runs.
Tangshan is named for a city in the Hebei province in northern
China. It was discovered at the Purple Mountain Observatory at
Nanking on 1979 December 14. Its last designation was 1979 XP
with its earliest designation being 1948 WL. Using the formula by
Harris (2003), the approximate diameter is 8 km when using the
MPCORB H value of 13.00 and albedo of 0.18. The principal
elements are: semi-major axis, 2.281AU; inclination, 4.616°; and
eccentricity 0.1212.
Figure 3 shows the 265 data points obtained on Nov. 26 and Nov.
28, 2003, that were used in the final period analysis. The synodic
period of the lightcurve is 3.461±0.020h and its amplitude is
0.25±0.03m, which yields a projected a/b axis ratio of 1.26:1 for
the assumed triaxial ellipsoid. The table below provides a
summary of the individual observation runs.
Figure 4. The lightcurve for 5076 Lebedev-Kumach. The synodic
period is 3.2190±0.0005h with an amplitude of 0.14±0.02m.
DATE
2003
Oct. 05
Nov. 15
Nov. 25
Phase
Angle
6.2
25.8
28.3
PAB
Long
2.3
8.8
11.6
Lat
1.1
–2.7
–3.5
Figure 3. The lightcurve for 2778 Tangshan. The data is phased
against a synodic period of 3.461±0.020h. The amplitude is
0.25±0.03m.
DATE
2003
Nov. 26
Nov. 28
Phase
Angle
2.5
3.3
PAB
Long
61.1
61.2
Lat
–3.4
–3.3
5076 Lebedev-Kumach
Discovered by L. I. Chernykh on 1973 September 26 at Nauchnyj,
Lebedev-Kumach is named for Vasilij Ivanovich LebedevKumach (1898-1949), prominent poet and song-writer, known for
his lyrical and patriotic verses for songs for many Soviet films.
The principal elements are: semi-major axis, 2.416AU;
inclination, 9.481°; and eccentricity 0.2327. Assuming an albedo
of 0.18 per Harris (2003) and the H value of 13.00 from the
MPCORB data file, the approximate diameter is 8 km.
Observations were obtained in October and November 2003, with
150 data points used in the final period analysis. The synodic
period of the lightcurve was found to be 3.2190±0.0005h and the
Figure 5. A phased lightcurve for (5892) 1981 YS1 using a
synodic period of 10.60±0.02h. The amplitude is 0.26±0.03m.
DATE
2003
Dec.
Dec.
Dec.
Dec.
Minor Planet Bulletin 31 (2004)
10
11
13
14
Phase
Angle
12.5
13.1
14.2
14.7
PAB
Long
64.0
64.2
64.6
64.8
Lat
–7.6
–7.6
-7.6
-7.5
39
Acknowledgments
(5892) 1981 YS1
This is another discovery from Purple Mountain Observatory at
Nanking (1981 December 23). The asteroid has also carried the
designations 1971 BS1, 1988 QG1, and 1988 UZ. Again using the
formula from Harris (2003) and assumed albedo of 0.18, the H
value of 13.60 gives an approximate diameter of 6 km. The
principal elements are: semi-major axis, 2.384AU; inclination,
4.585°; and eccentricity 0.3020.
358 observations obtained on four nights in December 2003 were
used to find a synodic period for the lightcurve of 10.60±0.02h
and amplitude of 0.26±0.03m. The latter implies a ratio of 1.27:1
for the projected a/b axes of a triaxial ellipsoid. Figure 5 shows a
phased plot of the observations and the table below gives a
summary for each run.
(6386) 1989 NK1
H.E. Holt discovered 1989 NK1 on 1989 July 10 at Palomar. It
has also been designated 1955 RG1 and 1991 FW4. Assuming an
albedo of 0.18, based on Harris (2003), and using the H value of
12.70 from the MPCORB table, the approximate diameter is 9 km.
The principal elements are: semi-major axis, 2.271AU;
inclination, 8.737°; and eccentricity 0.3008.
Observations were made in October and November 2003. The
211 data points used for analysis are shown in Figure 6 against the
derived synodic period of 3.1381±0.0005h. The amplitude of the
curve is 0.08±0.02m. This would give a ratio of 1.08:1 for the
projected a/b axes of a triaxial ellipsoid. The table below provides
the viewing aspects for each of the observation runs.
Thanks go to Dr. Alan Harris of the Space Science Institute for
making available the source code to his Fourier Analysis program
and his continuing support and advice. I also thank Robert D.
Stephens of Santana Observatory, Rancho Cucamonga, for his ongoing advice and support.
References
References Note: Asteroid names and discovery information are
from Schmadel (1999).
Harris, A.W., Young, J.W., Bowell, E., Martin, L.J., Millis, R.L.,
Poutanen, M., Scaltriti, F., Zappala, V., Schober, H.J., Debehogne,
H., and Zeigler, K.W., (1989). “Photoelectric Observations of
Asteroids 3, 24, 60, 261, and 863.” Icarus 77, 171-186.
Harris, Alan W. (2003). “Minor Planet Lightcurve Parameters.
On Minor Planet Center web site: http://cfawww.harvard.edu/iau/lists/LightcurveDat.html
Harris, Alan W. (2003a). Private communications.
Kozai, Y., (1979). “The dynamical evolution of the Hirayama
family.” In Asteroids (T. Geherels, Ed.) pp. 334-358. Univ. of
Arizona Press, Tucson.
Schmadel, L. (1999). Dictionary of Minor Planet Names, 4th
edition. Springer-Verlag, Heidelberg, Germany.
Tedesco, E. F., Tholen, D.J., and Zellner, B. (1989). “UBV colors
and IRAS alebedos and diameters”. In Asteroids II (R.P. Binzel,
T. Gehrels, and M.S. Matthews, Eds.), pp. 1090-1138. Univ. of
Arizona Press, Tucson.
Warner, B. D. (2003), “Lightcurve Analysis for [Several]
Asteroids”, Minor Planet Bulletin 30, 21-24.
CALL FOR OBSERVATIONS
Frederick Pilcher
Illinois College
Jacksonville, IL 62650 USA
Figure 6. A phased lightcurve for (6386) 1989 NK1 using a
synodic period of 3.1381±0.0005h. The amplitude is 0.08±0.02m.
DATE
2003
Oct.
Nov.
Nov.
Nov.
15
04
10
14
Phase
Angle
14.9
15.9
17.9
19.3
PAB
Long
27.1
31.4
32.8
33.8
Lat
-15.7
-15.4
-15.1
-14.8
Observers who have made visual or photographic measurements
of positions of minor planets in calendar 2003 are encouraged to
report them to this author on or before April 1, 2004. This will be
the deadline for receipt of reports which can be included in the
“General Report of Position Observations for 2003,” to be
published in MPB Vol. 31, No. 3.
Minor Planet Bulletin 31 (2004)
40
PHOTOMETRY OF 804 HISPANIA, 899 JOKASTE,
1306 SCYTHIA, AND 2074 SHOEMAKER
Date
Robert D. Stephens
11355 Mount Johnson Court
Rancho Cucamonga, CA 91737 USA
rstephens@foxandstephens.com
2003/10/07
2003/10/08
2003/10/09
2003/10/12
2003/10/13
(Received: 19 December)
Phase
Angle
4.9
4.8
4.8
4.9
5.1
PAB
(Long.)
16.4
16.4
16.4
16.4
16.4
PAB
(Lat.)
9.6
9.7
9.8
10.0
10.1
No.
Obs.
130
151
151
173
165
Table I: Observing circumstances for 804 Hispania
899 Jokaste
Results for the following asteroids (lightcurve period
and amplitude) observed from Santana Observatory
during the period September to December 2003 are
reported: 804 Hispania (14.845 ± 0.01 hours and 0.21
mag.), 899 Jokaste (6.245 ± 0.005 hours and 0.28 mag.),
1306 Scythia (15.05 ± 0.01 hours and 0.18 mag.), 2074
Shoemaker (57.02 ± 0.1 hours and 0.45 mag.).
899 Jokaste is a main-belt asteroid discovered August 3, 1918 by
M. Wolf at Heidelberg. It is probably named for a figure in the
opera Die Fledermaus by Johann Strauss. Three hundred one
observations over three sessions between November 27 and
December 3, 2003 were used to derive the synodic rotational
period of 6.245 ± 0.005 hours with an amplitude of 0.28 ± 0.02
magnitude. Table II gives the observed range of phase angles.
Santana Observatory (MPC Code 646) is located in Rancho
Cucamonga, California at an elevation of 400 meters and is
operated by Robert D. Stephens. Details of the equipment and
reduction techniques are found in Stephens (2003) and at the
author’s web site (http://home.earthlink.net/~rdstephens/
default.htm). All of the asteroids were selected from the “CALL”
web site “List of Potential Lightcurve Targets” (Warner 2003).
Shoemaker was selected because it is a Hungaria asteroid and
because it is named in honor of Eugene Shoemaker.
804 Hispania
Discovered March 20, 1915 by J. Comas Solá at Barcelona,
Hispania is a main-belt asteroid. Hispania is the Latin name of
Spain. Seven hundred sixty nine observations over five sessions
between October 7 and 13, 2003 were used to derive the synodic
rotational period of 14.845 ± 0.01 hours with an amplitude of
0.21 ± 0.02 magnitude. Table I gives the phase angles during the
observing run.
Figure 2: Lightcurve of 899 Jokaste based upon a derived period
of 6.245 ± 0.005 hours. Zero phase equals J.D. 2452975.801180
(corrected for light-time).
Date
2003/11/27
2003/12/02
2003/12/03
Phase
Angle
1.8
1.2
1.6
PAB
(Long.)
67.3
67.4
67.4
PAB
(Lat.)
1.9
1.5
1.4
No.
Obs.
104
73
124
Table II: Observing circumstances for 899 Jokaste
1306 Scythia
Figure 1: Lightcurve of 804 Hispania based upon a derived period
of 14.845 ± 0.01 hours. Zero phase is J.D. 2452920.867512
(corrected for light-time).
Discovered July 22, 1930 by G. N. Neuymin at Simeïs, Scthia is a
main-belt asteroid. It is named for the country of the ancient
Scythians, comprising parts of Europe and Asia in regions north
of the Black sea and east of the Aral Sea. Its estimated size is 34
km in diameter. Three hundred eighty four observations over
four sessions between September 23 and 30, 2003 were used to
derive the synodic rotational period of 15.05 ± 0.01 hours with an
amplitude of 0.18 ± 0.03 magnitude. Table III gives the phase
angles during the observing run.
Minor Planet Bulletin 31 (2004)
41
Figure 3: Lightcurve of 1306 Scythia based upon a derived
period of 15.05 ± 0.01 hours. Zero phase equals J.D.
2452908.860012 (corrected for light-time).
Date
2003/09/23
2003/09/26
2003/09/29
2003/09/30
Phase
Angle
9.1
8.5
8.1
8.0
PAB
(Long.)
12.5
12.5
12.6
12.6
PAB
(Lat.)
18.5
18.6
18.6
18.6
No.
Obs.
72
101
109
102
Table III: Observing circumstances for 1306 Scythia
2074 Shoemaker
2074 Shoemaker is a Hungaria asteroid discovered by E. Helin at
Palomar on October 17, 1974. It is named in honor of Eugene
Shoemaker (1928-1997). Based upon its H value, Shoemaker is
estimated to be between 4 and 9 km in size. Seven hundred
twenty two observations over nine nights between October 15 and
November 3, 2003 were used to derive the synodic rotational
period of 57.02 ± 0.10 hours with an amplitude of 0.45 ± 0.03
magnitude. Its long period made it very difficult to get adequate
overlap between the sessions. Each session contributed barely 10
percent to the lightcurve. Finally, the California wildfires, which
burned to within a half a kilometer of the observatory curtailed
observations until the asteroid was too low to observe. Because
the asteroid was moving so fast, each night had to be split into
two sessions with different comparison stars which were
corrected with zero point adjustments. Table IV gives the phase
angles during the observing run.
Figure 4: Lightcurve of 2074 Shoemaker based upon a derived
period of 57.02 ± 0.10 hours. Zero phase equals J.D.
2452929.762632 (corrected for light-time).
Date
2003/10/15
2003/10/16
2003/10/17
2003/10/18
2003/10/19
2003/10/20
2003/10/21
2003/10/23
2003/11/03
Phase
Angle
4.9
4.5
4.2
4.2
4.3
4.7
5.1
6.4
15.0
PAB
(Long.)
22.1
22.1
22.0
22.0
22.0
22.0
22.0
21.9
22.1
PAB
(Lat.)
5.7
5.3
4.9
4.4
4.0
3.6
3.2
2.4
-2.1
No.
Obs.
86
82
103
81
76
78
87
95
34
Table IV: Observing circumstances for 2074 Shoemaker
Acknowledgements
Many thanks to Brian Warner for his continuing work and
enhancements to the software program “Canopus” which makes it
possible for amateur astronomers to analyze and collaborate on
asteroid rotational period projects and for maintaining the CALL
Web site which helps coordinate collaborative projects between
amateur astronomers.
References
Stephens, R. D. (2003). “Photometry of 2134 Dennispalm, 2258
Viipuri, 3678 Mongmanwai, 4024 Ronan, and 6354 Vangelis.”
MPB 30, 46-48.
Stephens, R. D. (2003).
http://home.earthlink.net/~rdstephens/default.htm.
Warner, B. (2003). “Potential Lightcurve
http://www.minorplanetobserver.com/astlc.targets.
Minor Planet Bulletin 31 (2004)
Targets.”
42
CCD PHOTOMETRY OF 1248 JUGURTHA
Walter E. Worman
Department of Physics and Astronomy
Minnesota State University Moorhead
Moorhead, MN 56563
Michael P. Olson
Department of Physics
North Dakota State University
Fargo, ND 58105
(Received: 8 December
Revised: 11 January)
CCD observations were made of 1248 Jugurtha on four
nights in February and March 2002. The synodic period
of rotation was found to be 12.190 ± 0.002 hours with
the lightcurve amplitude evolving from 0.827 ± 0.017 to
0.734 ± 0.017 magnitudes. The period and large
amplitude are in agreement with previously reported
values.
the sum of the squares of the residuals. The resulting values were
a period of 12.190 ± 0.002 hours, the additive constant for the
second night was –0.0875, for the third night was –0.4719, and for
the fourth night was 0.3297 magnitudes. These are reasonable as
the uncertainties in the Hubble Guide Star Catalog are given to be
about ± 0.4 magnitudes. The standard deviation of the residuals
was 0.017 magnitudes, which is due to the amplitude difference of
the last night compared to the previous three.
A period of 12.190 hours was assumed and the second through
fourth night data were translated to fall on the first night data to
give the composite lightcurve shown in Figure 1. The time scale
is given in rotational phase with the zero corresponding to 0 hr on
February 17, 2002 UT. There are clearly two maxima and two
minima per rotation. The amplitude of the lightcurve is 0.827 ±
0.017 magnitudes for the first day and 0.734 ± 0.017 magnitudes
for the last day. The phase angle during the first three days of
observations varied between 8.9° and 7.3°, and the last day was
5.4°. We believe that this phase angle change is responsible for
the amplitude trend as less shadowing occurs on the asteroid at
smaller phase angles.
Reference
Observations
The asteroid 1248 Jugurtha is a main-belt asteroid with semimajor axis of 2.72 AU. Koff and Gross (2002) previously
reported a period of 12.1897 ±0.0001 hours with an amplitude in
excess of 0.70 magnitudes. The new observations of 1248
Jugurtha we report here were made at the Paul Feder Observatory,
located on the Buffalo River Site of the Minnesota State
University Moorhead Regional Science Center. Data were
collected on the nights of February 17, 21, 22, and March 10,
2002.
The observatory has a 16-inch computer controlled Cassegrain
telescope made by DFM. The associated Photometrics Star 1
CCD camera system was used to collect data. In all, 147 images
were made of the asteroid during the four nights. Of these, 141
were used in the analysis. The others were rejected because the
asteroid image was too close to another star or to dawn. The
exposures were 3 minutes long and typically separated by 10
minutes. No filter was used. Dark current and flat field
corrections were made to the data. Three stars were used as
magnitude standards for each image. The magnitudes were taken
from the Guide 7 program (Hubble Guide Star Catalog). A least
squares fit was done for each image and the relation between the
magnitude and the log of the total count determined. The
magnitude of the asteroid was then determined from this
relationship. A photometric aperture of 11 pixels by 11 pixels was
used and an equal sized region of the background nearby was used
for the background correction.
Koff, R.A. and Gross, J. (2002). “Lightcurve Photometry of
Asteroid 1248 Jugurtha.” MPB 29, 75-76
Figure 1. Rotational lightcurve for 1248 Jugurtha assuming a
period of 12.190 hours. The V magnitude scale is approximate
owing to the typical 0.4 mag. uncertainty of the Hubble Guide Star
Catalog.
Results
Times were corrected for travel time from the asteroid to the Earth
and were taken to be at the mid-times for the images. Lightcurves
were made for each of the four nights. Relative magnitudes from
night to night were uncertain as different comparison stars were
used. This was dealt with by using additive constants for the
second, third and fourth night magnitudes to bring them into
agreement with the first night. A single lightcurve for the four
nights was then least squares fit to a Fourier series including nine
harmonics. The additive constants for the second through fourth
nights and the period were then adjusted so that the fit minimized
Minor Planet Bulletin 31 (2004)
43
THE MINOR PLANET OBSERVER:
MAKING AND READING HISTORY
Brian Warner
Palmer Divide Observatory
17995 Bakers Farm Rd.
Colorado Springs, CO 80908
brian@MinorPlanetObserver.com
The news came in mid-October, 2003: the long lost minor planet
1937 UB, also known as Hermes, had been recovered. Brian Skiff
of the Lowell Observatory Near-Earth-Object Search (LONEOS)
program made the observations that sent astronomers, professional
and amateur, scurrying to their instruments. Within a few days,
radar and optical observations confirmed that the asteroid was
actually two separate bodies rotating around one another. You can
read more about the recovery at http://www.lowell.edu/press_
room/releases/recent_releases/Hermes_rls.html.
As often happens with the announcement of an NEO discovery or
recovery, there was a rush to gather as much data as possible. In
some cases, that amounted to “overkill” as the Minor Planet
Center received 50 or more astrometric observations a night in the
days immediately following recovery. That’s not meant to
discourage or disparage those who did turn in the observations.
Only to note that one wishes there could be such interest more
often, even when the targets are more mundane.
I was one of those who jumped into the rush to get optical
lightcurve data to support findings being reported by radar
imaging teams. Two teams of optical observers took the fore on
acquiring the data and analyzing it. One was lead by Petr Pravec
at Ondrejov Observatory, of which I was a part, and Raoul
Behrend of Geneva Observatory headed the other. A total of
about 15 observers from Europe, Australia, and the U.S.
contributed data that eventually lead to the finding of an orbital
period for the pair of about 13.9h with an amplitude of 0.07m.
The analysis further indicated that the objects appear to be locked
in synchronous rotation. It never ceases to amaze me that one can
make such determinations for asteroids based simply on the
changing brightness over time. The feat becomes even more
amazing when applied to eclipsing binary stars, which I’ve done
with the aid of the program, Binary Maker by David Bradstreet.
What the episode demonstrates is the value of cooperation and
collaboration among professionals and among professionals and
amateurs. Hermes was a difficult target, not so much because of
its brightness or motion across the sky but because of the low
amplitude of the curve and the uncertainty of the initial results.
This was one time where overwhelming the problem with data
was not a waste of time and effort but a strong necessity.
Most readers of these pages don’t need to be told that pro-am
collaborations can lead to a number of important discoveries and
continued advancement in many aspects of astronomy. There are
already many such collaborations among those involved in
asteroids and eclipsing binary stars. Those collaborations have
helped lead to some important developments in recent years and
will continue to do so. There are many amateurs available who
can and do high-level work every day (or night). The problem is
getting them tied up with professionals who can do the critical
analysis if they have the data.
annual meeting in Big Bear, CA, each year. The group changed
its name in 2003 and is working towards developing a method and
process – a network, if you will – to build a pool of high quality
observers and give professionals access to that pool. This parallels
the work that has long be done by the American Association of
Variable Star Observers (AAVSO) with whom SAS is trying to
work along with other groups. If you’d like more information on
SAS, visit their home page at http://www.socastrosci.org.
One of the pleasures I had while out working on Hermes and other
asteroids late in 2003 was to see a spectacular aurora. It’s rare to
see much, if anything, from my mid-latitude location in Colorado
but the heightened solar activity resulted in some spectacular
shows of bright green curtains, blood red sheets, rays of all lengths
and colors seen by those as far south as the southern tier of the
United States. Of course, one man’s treasure is another man’s
junk. Some Canadian amateurs were quick to point out that while
the show was nice, they see such displays quite often with many
so bright that the sky becomes is as if the quarter moon or more
was present. This brought to mind a time when I was doing some
visual variable star estimates and couldn’t figure out why the faint
variable suddenly disappeared. I looked up to see almost the
entire sky filled with sheet upon sheet of bright red aurora. I may
marvel at such a display now, but I’ll also wonder if a few
hundred miles north some other amateur is cursing Mother Nature.
I’ve been reading a very well done book called “Galileo’s
Daughter” by Dava Sobel (ISBN 0-8027-1343-2). It’s not new,
having been published in 1999, but if you haven’t had a chance to
read it, I recommend it very highly. It’s a tremendous and
touching insight into Galileo’s writings and times using in part
some or all of the 124 letters written by one of two of his
daughters, both of whom he placed in a convent before their
sixteenth birthday. It’s an unfortunate part of history that his
letters to her did not survive. The mother abbess of the convent
destroyed them soon after Suor Maria Celeste’s death in fear of
reprisals from the Church for having the materials of a declared
heretic.
I also managed to read – finally – Donald Yeoman’s book on
comets. This time I was about two decades behind the times. I
think what started the reading frenzy was getting bogged down in
the technical side of observing. It’s been a nice diversion to learn
a little more about the history and people in astronomy. It also
meant renewing a library card that was so old and infrequently
used that the library district didn’t think I was still alive. I was
glad to report such was the case and have rediscovered the joy of
just wandering through the library during my lunch hour from
time to time. There’s something old and something new around
every corner just waiting to be discovered.
With northern summer rapidly approaching, and so the asteroids
dipping well south of the celestial equator, I’ll be taking more time
to read some history, and traveling to one or more meetings. I
particularly look forward to the latter as it gives me a chance to
meet with some of you and learn how to improve my observing
and data analysis skills. I hope to see some new faces and help
develop new cooperative efforts among professionals and
amateurs. Let there be no doubt: the day of the amateur is far
from over despite the new large scopes and surveys coming on
line. Clear Skies!
Addressing this problem is just one goal of the Society for
Astronomical Sciences, formerly the IAPPP-West, which holds an
Minor Planet Bulletin 31 (2004)
44
LIGHTCURVES AND ROTATIONAL PERIODS OF
1474 BEIRA, 1309 HYPERBOREA, AND 2525 O'STEEN
Gordana Apostolovska
Institute of Physics, Faculty of Natural Sciences
1000 Skopje
Republic of Macedonia
gordanaa@iunona.pmf.ukim.edu.mk
Violeta Ivanova, Galin Borisov
Institute of Astronomy, Bulgarian Academy of Sciences
BG-1786 Sofia
Bulgaria
ivanova@astro.bas.bg, gborisov@astro.bas.bg
(Received: 15 January
On 21 September 2003, three days before Beira's particularly
favorable opposition, the asteroid was observed in B, V, R and I
bands. All frames were taken through a standard Johnson-Cousins
set of filters. The reduction to the BVRI standard system of the
asteroid magnitudes was made by means of the observations of
two standards fields SA114 and PG0231+051 (Landolt, 1992).
The atmospheric extinctions were kB=0.32±0.03, kV=0.15±0.02,
kR=0.140±0.036 and kI=0.07±0.01. The mean values of the color
indices of the asteroid were measured as: B-V=0.70±0.049,
V-I=0.687±0.012, R-I=0.314±0.006, and V-R=0.378±0.025.
Revised: 5 February)
The V-band lightcurves of the asteroids 1474 Beira,
1309 Hyperborea, 2525 O'Steen, and the mean color
indices for 1474 Beira are presented. The CCD
observations were carried out at the Bulgarian National
Astronomical Observatory Rozhen (MPC Code 071).
The calculated synodic periods are: 1474 Beira,
4.184±0.002h; 1309 Hyperborea, 13.95±0.02h; and
2525 O'Steen, 3.55±0.01h.
The observations we report for 1309 Hyperborea, 1474 Beira, and
2525 O'Steen were made at the Bulgarian National Astronomical
Observatory Rozhen (MPC Code 071). The data for Beira and
O'Steen were obtained with an SBIG ST-8E (Kodak KAF-1602E,
1536x1024px2, 1px=9µ m) CCD camera attached to a
0.50m/0.70m Schmidt telescope. A Photometrics CCD camera
(CE200A-SITe, 1024x1024, 1px=24µm) was used with the 2-m
RCC for observing of Hyperborea. Until our choice of these
objects, there was no reported information for photometric
observations of these asteroids in the list of Harris (2003).
In the preliminary reduction, images were dark and flat field
subtracted. The flat field correction with precision <1% was made
using twilight and dawn sky flat fields. The V-band lightcurves
were derived from the differential magnitudes between the
asteroid and comparison stars. Aperture photometry was
performed using the software program CCDPHOT (Buie, 1998).
For lightcurve analysis, we used Asteroid Catalog Software (APC)
(Magnuson et al. 1990), that produces composite lightcurves,
calculates rotational periods, and provides the Fourier analysis
fitting procedure of the lightcurve, which we used.
1474 Beira
Beira is a Mars-crossing asteroid with a semi-major axis of 2.74
AU, eccentricity 0.49 and inclination of orbit 26.7 degrees. Beira
was discovered in 1935 by C. Jackson in Johannesburg. The
assumed diameter of Beira in the IRAS Minor Planet Survey,
(Tedesco, 1992) is 39 km. The Tholen taxonomic type (Tholen,
1989) is FX. At the time of observation asteroid was at 14.6m and
the solar phase angle was 31.5 degrees. On 24 and 25 of August
2003, Beira was observed for about 6 hours, an interval that was
more than the full lightcurve coverage. We determined the
synodic period to be 4.184±0.002 hours. The amplitude of the
composite lightcurve, Fourier fitted of order 6, is 0.149±0.010
magnitude. The obtained composite lightcurve has maxima and
minima which slightly differ from each other by shape and height.
Figure 1: Lightcurve of 1474 Beira based on a period of
4.184±0.002 hours.
Figure 2: Lightcurve of 1309 Hyperborea based on a period of
13.95±0.014 hours.
(1309) Hyperborea
Hyperborea is a main-belt asteroid discovered in 1931 by G. N.
Neujmin in Simeis. It has a semi-major axis of 3.20 AU,
eccentricity 0.15 and inclination of orbit 10.28 degrees. The
diameter of Hyperborea is 59 km (Tedesco, 1992). The
observations of this asteroid at Rozhen were carried out in two
nights: 12 and 14 January 2002. On the first night, bad weather
conditions permitted only 2 hours of observations. The second
night of observations cover 7.5 hours of the lightcurve, which
reveals a nice maximum and very sharp minimum. Assuming a
standard lightcurve with two pairs of symmetrical extrema we
estimate a period of 13.95±0.02 hours. The amplitude of the
Minor Planet Bulletin 31 (2004)
45
composite lightcurve for the presented phase interval is about 0.4
magnitude.
Tholen, D. J., (1989). “ Asteroid taxonomic classifications.” In
Asteroids II (R. P. Binzel, T. Gehrels, and M. S. Matthews, Eds.),
pp 1139-1150. Univ. Arizona Press, Tucson.
(2525) O'Steen
This asteroid was discovered in 1981 by B. A. Skiff in Flagstaff at
the Anderson Mesa Station. O'Steen is a main-belt asteroid with a
semi-major axis of 3.13 AU, eccentricity 0.195 and inclination of
orbit 2.78 degrees. The assumed diameter of 2525 O’Steen is 106
km (Tedesco, 1992). O'Steen was observed on 23 of September
2003. In the time of the observation the asteroid was 14m and the
solar phase angle was 6.98 degrees. One night observations with a
duration of 6 hours covered more than one cycle of the asteroid.
The composite lightcurve based on a synodic period of 3.55±0.01
hours is asymmetric. The amplitude of the composite lightcurve,
Fourier fitted of order 4, is 0.193±0.009 magnitude.
BOOK REVIEW
Richard P. Binzel, Editor
A Practical Guide to Lightcurve Photometry and
Analysis by Brian D. Warner. Bdw Publishing, 2003.
ISBN 0-9743849-0-9, paperback, 266 pages. (Price
$30, available at www.MinorPlanetObserver.com)
Oh how long we have waited for a book like this! In the distant
past, amateurs had to crack their way into the field of lightcurve
photometry by tackling papers such as Hardie (1959) and by
building their own photometers following the classic book by
Frank Bradshaw Wood (1963). Several follow-on books that
carried the field forward were published by Willmann-Bell, Inc.,
including Genet (1983) and Henden and Kaitchuck (1990). The
affordability, proliferation, and enabling capabilities of CCD
cameras at “amateur” observatories has opened a huge potential
for new opportunities for new observers to make valuable
lightcurve photometry measurements. Yet a void has existed in
detailing how to get started and carry forward a program of
lightcurve photometry driven by scientific curiousity.
Figure 3: Lightcurve of 2525 O'Steen based on a period of 3.55±
0.01 hours. The Fourier fit of order 4 is presented with solid line.
Acknowledgments
This research was supported by contract Num, NZ-904/99 with the
National Science Fund, Ministry of Education and Sciences,
Bulgaria and by contract with the Ministry of Education and
Science, Republic of Macedonia.
References
Buie, M. W., (1998). http://www.lowell.edu/users/buie/idl
/ccdphot.html
Harris, A. W. (2003). “Minor Planet Lightcurve Parameters”. On
the Minor Planet Center website: http://cfa-www.harvard.edu
/iau/lists/LightcurveDat.html (updated October 2003)
Landolt, A.U., (1992). “UBVRI Photometric standard stars in the
magnitude range 11.5<V<16.0 around the celestial equator”.
Astron. J. 104, 340-491
Magnuson , P. and Lagerkvist, C. I., (1990). “Analyses of
asteroid lightcurves. I. database and basic reduction.” Astron.
Astrophys. Suppl. Ser. 86, 45-51
Tedesco, E., F. (Ed.), 1992. IRAS Minor Planet Survey, (Phillips
Laboratory Technical Report No. PL-TR-92-2049. Hanscom Air
Force Base, MA)
Brian D. Warner’s Practical Guide now fills that void. It is
written from the perspective of one who still remembers what it
was like to start as a beginner. Thus the writing comes across in a
warm and welcoming style. Much advice comes from Warner’s
own experience, building upon works like Henden and Kaitchuck
(1990), and it is conveyed as being told from one friend to
another. It is hard to imagine any new person who picks up this
book with genuine interest being able to resist taking the author’s
extended hand and gently being guided forward. Warner first
coaxes his readers to take the plunge by tantalizing them with the
science that comes out of the observations. Those who try CCD
lightcurve photometry because of the technical challenge will do it
once or twice and then move to the next challenge elsewhere.
This book’s approach is to capture you for the long term by
getting you hooked on the joy and satisfaction of learning and
contributing new scientific knowledge about our Universe. It is
this common passion for new knowledge that erases barriers
between “amateur” and professional astronomers. There are no
barriers here.
About 40 pages of the book are devoted to communicating the
fundamentals of photometry, and this is accomplished with the
clear and concise skill of a patient and expert teacher. Many
references here (and in the book’s Bibliography) tell you where to
go for more depth than this overview allows. Technical terms are
given in italics when first introduced and a nice (although limited
in length) Glossary is given at the end for additional help.
Throughout the book, text blocks are offset within boxes
displaying the subheading “Tying It Together…” to try to keep the
big picture in mind while focusing on the details. Because
computers and software are so intertwined with CCD data
collection and reduction, the bulk of this book provides a guide to
how to use these tools. While Warner himself has developed a
wide variety of excellent and popular software tools, he does not
exclusively tout his own packages. Most importantly, the author
Minor Planet Bulletin 31 (2004)
46
tries to convey an understanding of what the various reduction
steps are intended to accomplish. Numerous correct and fully
warranted cautionary statements are made not to place blind trust
in the output of these packages, but to give careful human thought
as to whether the results being spit out make sense. The copious
examples serve to help a beginner to learn rapidly many of the
most common pitfalls. Ultimately it is the experience that the new
observer gains with her/his own data that brings about confidence
and expertise.
Brian D. Warner’s Practical Guide is an instant classic and
required reading for anyone learning the ropes of CCD photometry
and its application to the challenge of lightcurve observations of
both asteroids and variable stars. More than any other volume in
the past decade, this book will spark new interest and new
observers to the field of lightcurve studies. Thank you Brian for
illuminating the way. We welcome all who follow.
New observers who are ready to start their own programs will find
advice on how to get off the ground and choose targets to begin
working on. Recognizing that the higher purpose is to
communicate one’s results, one of the final sections of the book
describes the task and venues for publication, including the Minor
Planet Bulletin. Many details and technical examples are saved
for the Appendices, making the main body of the text smoothly
flowing and readable. Finally the inclusion of standard star fields,
reprinted with permission, puts some enormously useful reference
material into a single accessible place. The quality and clarity of
the printing of the standard star charts enables excellent
photocopies of these pages – for personal use and handling ease at
the telescope or computer screen.
Genet, R. M. (1983). Solar System Photometry Handbook.
Willmann-Bell, Inc., Richmond, VA.
LIGHTCURVE PHOTOMETRY OPPORTUNITIES
APRIL – JUNE 2004
For many years, the thrust of this article has been to get
lightcurves on any object since the number of well-established
lightcurve parameters was woefully small. The list of spin axis
values was nearly non-existent. In recent years, there has been a
dramatic increase in the number of entries on both lists, which are
just now beginning to tell part of the tale of the true evolution of
the asteroid system. This is no time to rest on our laurels but, with
the promise of even more exciting and important discoveries to be
made for the want of more observations, to reinforce our
determination. Again, let there be no doubt that observations will
be put to use. The fear that they will be lost in the dark chasms of
time and neglect should be put aside.
Brian D. Warner
Palmer Divide Observatory
17995 Bakers Farm Rd.
Colorado Springs, CO 80908
Mikko Kaasalainen
Rolf Nevanlinna Institute
P.O. Box 4 (Yliopistonkatu 5, room 714)
FIN-00014 University of Helsinki
Finland
References
Hardie, R. H. (1959). “An Improved Method for Measuring
Extinction.” Astrophys. J. 130, 663-669.
Henden, A. and Kaitchuck, R. (1990). Astronomical Photometry.
Willmann-Bell, Inc., Richmond, VA.
Wood, F. B. (1963).
Macmillan, New York.
Photoelectric Astronomy for Amateurs.
So that neither goal – more raw lightcurves and curves for
shape/axis studies – is neglected, we’re including two lists. The
first contains asteroids that have no or poorly established
parameters. Note that this time around we’ve included a number
with at least preliminary values, some with very long periods.
These are challenging, no doubt, but no less important than a
passing NEO spinning several times an hour. In fact, they may be
more important right now since the slow rotators are, for a large
part, the greatest mystery in the study of spin rates.
Alan W. Harris
Space Science Institute
4603 Orange Knoll Ave.
La Canada, CA 91011-3364
Petr Pravec
Astronomical Institute
CZ-25165 Ondrejov
Czech Republic
ppravec@asu.cas.cz
Spinning “flat hamburgers”, “potatoes”, and “footballs” are often
used to describe an asteroid when explaining its lightcurve. Even
the human head can give a reasonable approximation to some
lightcurves – assuming the person is not bald! The point is that
asteroids come in all sorts of shapes and sizes and that it’s
becoming increasingly important to determine the shapes and
orientation of the spin axis for as many asteroids as possible.
A recent review of the known lightcurves and spin axes shows an
almost certain influence of the YORP effect on the spin rates and
orientations of asteroids less than about 40km in size. The exact
shape, or good approximation, of the asteroid is important since
the influence of the YORP effect is most powerful when the object
is highly irregular in shape.
The second list should be of help for those with smaller
instruments. They are relatively bright and so should be within
easy reach. These objects are only a small number of well done
lightcurves away from having their shape and/or spin axis
resolved, or at least reasonably known. Those working objects on
this list should contact co-author Mikko Kaasalainen to coordinate
their efforts with his and to be sure that the object has not since
been observed well enough to have been modeled.
Important Notes: 1) The periods that are listed should be
considered preliminary. Don’t be overly influenced by them and
try to force your results to the same or similar values. Let the data
dictate the solution, not vice versa. 2) The Declination is actually
for when the asteroid is brightest. In most cases, it is about the
same for when at opposition.
Minor Planet Bulletin 31 (2004)
47
You’ll find a more complete list of lightcurve opportunities for the
current and recent quarters on the CALL web site.
(http://www.MinorPlanetObserver.com/astlc/default.htm). Be
sure to check the link on the CALL site to planned radar
observations. Optical observations are often needed to support the
radar work.
Lightcurve Opportunities
#
498
168
203
744
265
566
143
755
1605
738
1109
407
680
863
613
1728
1143
1994
6669
1353
478
2091
2957
159
582
4558
839
227
3089
427
12008
1246
780
1274
426
749
275
954
696
9601
1031
1738
Name
Tokio
Sibylla
Pompeja
Aguntina
Anna (F)
Stereoskopia
Adria
Quintilla (F)
Milankovitch
Alagasta
Tata
Arachne
Genoveva
Benkoela
Ginevra
Goethe Link
Odysseus
Shane
Obi
Maartje
Tergeste
Sampo
Tatsuo (F)
Aemilia
Olympia
Janesick
Valborg
Philosophia (F)
Oujianquan (F)
Galene
1996 TY9 (F)
Chaka
Armenia
Delportia
Hippo
Malzovia (F)
Sapientia
Li
Leonora
1991 UE3 (F)
Arctica
Oosterhoff
Opposition
Date
Mag
4 06.2 13.4
4 06.1 12.9
4 06.0 12.6
4 11.2 14.1
3 30.2 13.4
4 14.2 13.3
4 09.2 12.7
4 17.1 13.3
4 19.7 14.5
4 19.5 14.0
4 17.0 14.2
4 16.5 12.8
4 23.9 12.7
5 06.7 13.9
5 09.5 14.1
5 12.1 14.1
5 14.0 15.0
5 18.6 14.9
5 19.2 14.2
5 21.3 14.4
5 21.8 12.3
5 24.8 14.8
5 27.9 13.9
5 30.8 12.8
6 07.0 14.0
5 28.2 14.2
5 26.6 13.5
6 02.2 12.2
6 06.1 14.0
6 06.1 13.4
5 31.1 12.7
6 07.9 13.9
6 13.5 13.8
6 16.2 13.9
6 17.7 12.7
6 20.3 13.2
6 21.2 12.5
6 23.1 13.4
6 26.3 14.0
6 30.9 13.9
6 30.3 14.3
6 30.2 13.7
Dec
+ 8
- 8
- 9
+ 2
-46
- 4
-23
- 8
- 2
- 6
-16
-22
-10
+21
-27
-20
-18
-22
-22
-14
-18
- 7
-22
-14
+20
-27
-43
-37
-16
-28
-34
-38
+ 2
-31
-45
-19
-18
-22
-31
-29
+ 0
-32
Per
Amp
>20.
>0.36
23.82 >0.30
46.6 >0.10
17.
11.
0.08
13.29
0.15
44.
0.45
16.45
0.63
>12.
25.?
0.11
>0.1
15.
71.3
0.2
0.38
25.
36.0
100.
>0.2
>0.6
>0.11
Name
Frigga
Aurelia
Astraea
Danby
Desiderata
Atalante
Bathilde
Hansa
Shaposhnikov
Nemausa
Patientia
Doris
Adelheid
Papagena
Freia
Themis
Siegena
Opposition
Date
Mag
Dec
4 04.3 12.3 -07
4 20.2 10.6 -14
4 28.6
9.8 -05
5 01.3 17.3 -16
5 06.0
9.8 -15
5 10.5 13.8 -40
5 15.2 12.5 -23
5 19.4 11.8 -19
5 25.5 14.5 -23
5 28.7 10.3 -05
5 30.8 11.3 -14
5 31.9 11.6 -13
6 01.7 13.4 -02
6 05.9 11.3 -19
6 09.0 13.3 -21
6 18.3 11.6 -24
6 21.7 12.1 +06
The Minor Planet Bulletin is open to papers on all aspects of
minor planet study. Theoretical, observational, historical, review,
and other topics from amateur and professional astronomers are
welcome. The level of presentation should be such as to be
readily understood by most amateur astronomers. The preferred
language is English. All observational and theoretical papers will
be reviewed by another researcher in the field prior to publication
to insure that results are presented clearly and concisely. It is
hoped that papers will be published within three months of receipt.
However, material submitted by the posted deadline for an issue
may or may not appear in that issue, depending on available space
and editorial processing.
The MPB will not generally publish articles on instrumentation.
Persons interested in details of CCD instrumentation should join
the International Amateur-Professional Photoelectric Photometry
(IAPPP) and subscribe to their journal. Write to: Dr. Arnold M.
Heiser, Dyer Observatory, 1000 Oman Drive, Brentwood, TN
37027 (email: heiser@astro.dyer.vanderbilt.edu). The MPB will
carry only limited information on asteroid occultations because
detailed information on observing these events is given in the
Occultation Newsletter published by the International Occultation
Timing Association (IOTA). Persons interested in subscribing to
this newsletter should write to: Art Lucas. Secretary & Treasurer,
5403 Bluebird Trail, Stillwater, OK 74074 USA
(business@occultations.org). Astrometry measurements should be
submitted to the IAU Minor Planet Center and are no longer being
published or reproduced in the MPB.
Manuscript Preparation
>20.
>0.2
>32.
0.15
>20.
14.
>0.05
0.2
51.0
>0.22
Shape/Axis Opportunities
#
77
419
5
3415
344
36
441
480
1902
51
451
48
276
471
76
24
386
INSTRUCTIONS FOR AUTHORS
Per
(h)
9.012
16.709
16.800
2.851
10.77
9.93
10.447
5.324
21.2
7.783
9.727
11.89
6.328
7.113
9.972
8.374
9.763
Amp.
0.07-0.19
0.08
0.10-0.30
0.09-0.14
0.17
0.15-0.17
0.13
0.29
0.42
0.10-0.14
0.05-0.10
0.35
0.07-0.10
0.11-0.13
0.10-0.33
0.09-0.14
0.11
It is strongly preferred that all manuscripts be prepared using the
template found at: http://www.minorplanetobserver.com/astlc/
default.htm Manuscripts should be less than 1000 words. Longer
manuscripts may be returned for revision or delayed pending
available space. For authors not using the template noted above,
manuscripts may be submitted electronically as ASCII text or on
paper as a typescript. Typescripts should be typed double spaced
and consist of the following: a title page giving the names and
addresses of all authors (editorial correspondence will be
conducted with the first author unless otherwise noted), a brief
abstract not exceeding four sentences, the text of the paper,
acknowledgments, references, tables, figure captions, and figures.
Please compile your manuscripts in this order.
For lightcurve articles, authors are encouraged to combine as
many objects together in a single article as possible. For general
articles, the number of tables plus figures should not exceed two.
Tables should be numbered consecutively in Roman numerals,
figures in Arabic numerals. We will typeset short tables, if
necessary. Longer tables must be submitted in “camera ready”
format, suitable for direct publication. Font size should be large
enough to allow for clear reproduction within the column
dimensions described below. We prefer to receive figures in
electronic format, 300 dpi or higher quality, black markings on
white. Because of their high reproduction cost, the MPB will not
print color figures. Labeling should be large enough to be easily
readable when reproduced to fit within the MPB column format.
If at all possible, you are strongly encouraged to supply tables and
figures at actual size for direct reproduction. Tables and figures
intended for direct reproduction to occupy one-half page width
should be 8.6 cm wide, or full-page width, 17.8 cm. Size your
tables and figures to fit one-half page width whenever possible.
Minor Planet Bulletin 31 (2004)
48
Limit the vertical extent of your figures as much as possible. In
general they should be 9 cm or less.
References should be cited in the text such as Harris and Young
(1980) for one or two authors or Bowell et al. (1979) for more
than two authors. The reference section should list papers in
alphabetical order of the first author’s last name. The reference
format for a journal article, book chapter, and book are as follows:
Harris, A.W., Young, J.W., Bowell, E., Martin, L. J., Millis, R. L.,
Poutanen, M., Scaltriti, F., Zappala, V., Schober, H. J.,
Debehogne, H, and Zeigler, K. (1989).
“Photoelectric
Observations of Asteroids 3, 24, 60, 261, and 863.” Icarus 77,
171-186.
Pravec, P., Harris, A. W., and Michalowski, T. (2002). “Asteroid
Rotations.” In Asteroids III (W. F. Bottke, A. Cellino, P.
Paolicchi, R. P. Binzel, eds.) pp 113-122. Univ. Arizona Press,
Tucson.
Warner, B. D. (2003). A Practical Guide to Lightcurve
Photometry and Analysis. Bdw Publishing, Colorado Springs,
CO.
Authors are asked to carefully comply with the above guidelines
in order to minimize the time required for editorial tasks.
Submission
All material submitted for publication in the Minor Planet Bulletin
should be sent to the editor: Dr. Richard P. Binzel, MIT 54-410,
Cambridge, MA 02139, USA (email: rpb@mit.edu). Authors are
encouraged to submit their manuscripts electronically as email
attachments or as ASCII text, prepared following the instructions
above. Alternatively, your article may be sent by post on diskette
(all diskettes must be accompanied by a complete printed copy of
all material) or as a typed manuscript. When sending material by
post, please include high quality original printed figures and tables
that can be directly reproduced. In most cases, proofs of articles
will be sent to authors prior to publication.
THE MINOR PLANET BULLETIN (ISSN 1052-8091) is the quarterly
journal of the Minor Planets Section of the Association of Lunar and
Planetary Observers. The Minor Planets Section is directed by its
Coordinator, Prof. Frederick Pilcher, Department of Physics, Illinois
College, Jacksonville, IL 62650 USA (pilcher@hilltop.ic.edu), assisted by
Lawrence Garrett, 206 River Road, Fairfax, VT 05454 USA
(Lgasteroid@globalnetisp.net). Richard Kowalski, 7630 Conrad St.,
Zephyrhills, FL 33544-2729 USA (qho@bitnik. com) is Associate
Coordinator for Observation of NEO’s, and Steve Larson, Lunar and
Planetary Laboratory, 1629 E. University Blvd., University of Arizona,
Tucson, AZ 85721 USA (slarson@lpl.arizona.edu) is Scientific Advisor.
The Asteroid Photometry Coordinator is Brian D. Warner, Palmer Divide
Observatory, 17995 Bakers Farm Rd., Colorado Springs, CO 80908 USA
(brian@MinorPlanetObserver.com).
The Minor Planet Bulletin is edited by Dr. Richard P. Binzel, MIT 54-410,
Cambridge, MA 02139 USA (rpb@mit.edu) and is produced by Dr. Robert
A. Werner, JPL MS 301-150, 4800 Oak Grove Drive, Pasadena, CA 91109
USA (robert.a.werner@jpl.nasa.gov). Derald D. Nye serves as the
distributor.
The staff of the Minor Planet Section invites MPB subscribers who are not
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Minor Planet Bulletin
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Articles for submission to the MPB should be sent to the editor. All
authors should follow the guidelines given in “Instructions for Authors” in
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The deadline for the next issue (31-3) is April 15, 2004. The deadline for
issue 31-4 is July 15, 2004.
Minor Planet Bulletin 31 (2004)