The discovery that 2003 QY90 is a possible binary TNO was announced in
by Elliot et al. in IAUC 8235. The object appears elongated in
ground-based images (0.5 arcsec seeing) taken over a
1.9 hour interval. Image analysis suggests two components of
comparable brightness with separation of arcsec
If you were unable to attend the KBO occultation workshop at the DPS
meeting, most of the presentations are available online at:
Recently, a couple readers submitted fascinating, pre-publication
images of EKOs that may resolve some outstanding issues of the Kuiper
belt (e.g., the bimodality of the color distribution and if there is
an ``edge'' or not) and even show evidence of organic compounds. I
have created a new webpage for such images if any other newsletter
readers would like to submit their own:
There were 9 new TNO discoveries announced since the previous issue of Distant EKOs:
2003 QW111, 2003 QX111, 2003 QY111, 2003 QZ111, 2003 QA112, 2003 QB112, 2003 QE112, 2003 UY117, 2003 UZ117
and 7 new Centaur/SDO discoveries:
2003 QC112, 2003 QD112, 2003 QN112, 2003 QP112, 2003 QM112, 2003 QO112, 2003 UA118
2003 QA91 (TNO SDO)
2003 QY90 (TNO SDO)
Objects recently assigned numbers:
1999 OF4 = (66452)
1999 RZ253 = (66652)
2002 PP149 = 2000 QM252
2002 VQ94 removed from list of SDOs, now identified as C/2002 VQ94 (LINEAR)
Current number of TNOs: 728 (and Pluto & Charon, and 10 other TNO binary companions)
Current number of Centaurs/SDOs: 140
Current number of Neptune Trojans: 1
Out of a total of 869 objects:
437 have measurements from only one opposition
325 of those have had no measurements for more than a year
188 of those have arcs shorter than 10 days
(for more details, see:
We analyze visible, infrared, radio and spectroscopic observations of 2060 Chiron in a synthetic way to determine the physical properties of its nucleus. From visible observations performed from 1969 to 2001, we determine an absolute V magnitude for the nucleus of with an amplitude of 0.160.03, implying a nearly spherical nucleus with a ratio of semi-axes . Infrared observations at 25, 60, 100 and 160 m (i.e., covering the broad maximum of the spectral energy distribution) obtained with the Infrared Space Observatory Photometer (ISOPHOT) in June 1996 when Chiron was near its perihelion are analyzed with a thermal model which considers an intimate mixture of water ice and refractory materials and includes heat conduction into the interior of the nucleus. We find a very low thermal inertia of 3+5-3 JK-1m-2s-1/2 and a radius of 715 km. Combining the visible and infrared observations, we derive a geometric albedo of 0.110.02. We find that the observed spectra of Chiron can be fitted by a mixture of water ice () and refractory () grains, and that this surface model has a geometric albedo consistent with the above value. We also analyze the visible, infrared and radio observations of Chariklo (1997 CU26) and derive a radius of km, a geometric albedo of 0.070.01 and a thermal inertia of 0+2-0 JK-1m-2s-1/2. A mixture of water ice () and refractory () grains is compatible with the near-infrared spectrum and the above albedo.
To appear in: Astronomy & Astrophysics
For preprints, contact Olivier.Groussin@dlr.de
We report visible spectroscopy of the two largest known trans-Neptunian objects (TNOs): Quaoar (=50000) and Ixion (=28976) obtained respectively on 4th and 5th May 2003 with the ESO New Technology Telescope (NTT) at La Silla, Chile. The spectrum of Ixion is moderately red with an absorption feature around 0.80 m, while Quaoar is a red object with a featureless spectrum. These differences seem to indicate differences in primordial composition or dynamical history, in spite of their present similar orbits.
Published in: Astronomy & Astrophysics, 408, L17 (2003 September)
For preprints, contact email@example.com
We present optical observations of 24 Centaurs performed between 1998 and 2002 with the University of Hawaii 2.2-m telescope. This is the largest such Centaur survey to date. We report colors for all objects, and show that they cover a continuum with mean V-R color of and standard deviation 0.15. The color distribution fits between those of the Kuiper Belt and the cometary nuclei, and seems consistent with the dynamical concept of the majority of Centaurs originating from the Kuiper Belt. We find no strong correlation between a Centaur's color and its orbital elements; there is at best a correlation with semimajor axis, with redder Centaurs being farther from the Sun. We have calculated the phase-darkening slope parameters G for 5 Centaurs, 4 of which are reported for the first time. They range from -0.18 to 0.13. We have sufficient data to constrain the rotation periods of two Centaurs, 1999 UG5 (which we reported earlier) and 1998 SG35. We performed a comparison of the surface brightness profiles of 10 apparently-inactive Centaurs with point sources. We found no coma around these 10 objects, including C/LINEAR (2000 B4), and generally the upper limits to the dust mass loss rates are below 0.05 kg s-1.
To appear in: Icarus
For preprints, contact firstname.lastname@example.org
We report the conditions and results of an observation campaign organized in 2000 September at the Pic du Midi Observatory, and dedicated for the first time to the study of Kuiper belt objects (KBOs) by stellar occultations. The observation consisted of recording the flux of a well-chosen star with a fast photometer (20 Hz) and counting occultations of this star by passing KBOs. The campaign provided 15 hr of good-quality signal (rms ) and zero detections of KBOs at a 4 detection level. For a KBO differential size distribution assumed to vary as r-q, this first result suggests a slope . A refined analysis of the data, studying diffraction patterns, allowed us to find an event at a 3 detection level compatible with a 150 m KBO. More generally, observation campaigns of stellar occultation by KBOs on 2 m class telescopes could statistically constrain the slope and the expected turnover radius due to collisional erosion of the subkilometer KBO size distribution.
Published in: The Astrophysical Journal Letters, 594, L63 (2003 September 1)
For preprints, contact Francoise.Roques@obspm.fr
We present the results of optical observations of C/NEAT (2001 T4), taken on 3 dates between October 2001 and September 2002, at the University of Hawaii 2.2 meter telescope. Coma was present for each observation, but the activity level was variable. We present surface brightness profiles, dust production rates and evidence for structure in the coma. There is a radial gradient in coma color, with the outer coma exhibiting the bluest colors. The object's V-R and R-I colors indicate that this is one of the reddest objects with a Centaur-type orbit.
Published in: Publications of the Astronomical Society of the Pacific, 115, 981
For preprints, contact email@example.com
The peculiar relationship of Pluto to Neptune, its resonances and high eccentricity and inclination, have led to the theory that the relationship arose from the migration of the outer planets, particularly the outward migration of Neptune, during the early solar system. In support of this scenario is the fact that the formation of Neptune at its current location would have been complicated by long dynamical times and low densities in the solar nebula. Here we address the following questions: Though the formation of Neptune at its current location seems unfavorable, are there dynamical obstacles to the capture of Pluto and the Plutinos under this scenario? Or are there features of the Neptune-Pluto system that would allow us to preclude this possibility of Neptune forming near its current orbit? Levison & Stern have examined the effect of the purely gravitational interactions of the giant planets on Pluto and concluded that the most important dynamical aspects of the Neptune-Pluto system could be reproduced. The exception was the amplitude of the 3:2 resonant argument, which was found to be too large in their model. We performed simulations of the outer solar system that included a slowly accreting Neptune and found that the efficiency of capture of dynamically cold particles into the 3:2 resonance was increased by a factor of 3, and that the resonant argument was substantially decreased. However, further dissipation is still required to match all aspects of the Plutino population and to produce truly Pluto-like orbits. Given that cold initial conditions did not reproduce the observations completely, simulations of initially dynamically hot particles near the 3:2 resonance with Neptune were also examined. These results, though resulting from seemingly ad hoc starting conditions, are reported as they produce remarkably good matches with both the Plutino population and Pluto's own orbit, including all three of its known resonances. These simulations reveal that Pluto could have arisen from an initially low-e (0) but high-i (25) orbit, both a clue to its origin and an illustration of the difficulty in understanding Pluto's current orbital configuration.
Published in: The Astronomical Journal, 126, 1575 (2003 September)
For preprints, contact firstname.lastname@example.org
The orbital evolution and stability of planetary systems with interaction from the belts is studied using the standard phase-plane analysis. In addition to the fixed point which corresponds to the Keplerian orbit, there are other fixed points around the inner and outer edges of the belt. Our results show that for the planets, the probability to move stably around the inner edge is larger than the one to move around the outer edge. It is also interesting that there is a limit cycle of semi-attractor for a particular case. Applying our results to the Solar System, we find that our results could provide a natural mechanism to do the orbit rearrangement for the larger Kuiper Belt Objects and thus successfully explain the absence of these objects beyond 50 AU.
To appear in: International Journal of Bifurcation and Chaos
For preprints, contact email@example.com
or on the web at
Mean motion resonances (MMRs) can lead either to chaotic or regular motion. We report on a numerical experiment showing that even in one of the most chaotic regions of the Solar System, the region of the giant planets, there are numerous bands where MMRs can stabilize orbits of small bodies in a time span comparable to their lifetimes. Two types of temporary stabilization were observed: short period ( years) when a body was in a MMR with only one planet and long period (over 105 years) when a body is located in overlapping MMRs with two or three planets. The experiment showed that the Main Belt region can be enriched by cometary material in its pre-active state due to temporary resonant interactions between small bodies and giant planets.
Published in: Astronomy & Astrophysics, 405, 1145 (2003 July)
For preprints, contact firstname.lastname@example.org
We present a simple method for constraining the possible future positions of distant solar system objects observed twice over only a very short time span. The method involves taking two positions and then determining a large number of possible orbits compatible with the observed motion across the sky for an object with unknown (but constrainable) distance from Earth. A key advantage of this approach is that it assumes only that the object is bound and distant. Monte Carlo techniques are used to incorporate astrometric uncertainty and map out the allowed orbital parameter space. The method allows us to compute the object's position on the selected recovery date for each potential orbit, assisting the selection of fields for recovery observations. Examples are shown, and usage of the code is discussed.
Published in: Publications of the Astronomical Society of the Pacific, 115, 1330
For preprints, contact email@example.com
The source code is available at
Simultaneous Visible and Near-infrared Time-resolved
Observations of the Outer Solar System Object (29981) 1999 TD10
B.E.A. Mueller1, C.W. Hergenrother2, N.H. Samarasinha1,
H. Campins2,3, and D.W. McCarthy, Jr.4
1 NOAO, Tucson AZ, USA
2 LPL, Univ. of AZ, Tucson AZ , USA
3 Univ. of Central Flordia, Orlando FL, USA
4 Steward Obs., Univ. of AZ, Tucson AZ, USA
Submitted to: Icarus
For preprints, contact firstname.lastname@example.org
The 3rd Zone: Exploring the Kuiper Belt
1 SwRI, 1050 Walnut St., Suite 400, Boulder, CO. 80302, USA
Sky & Telescope, 106, 30 (2003 November)
For preprints, contact email@example.com
Only a theory ten years ago, the Edgeworth-Kuiper Belt is now a reality, with a continuously increasing number of discovered objects. The Kuiper Belt Objects are attracting a growing interest from a wide scientific community. They not only are thought to be the source of many short period comets, but also they should be formed by almost pristine materials, whose study is of extreme interest for the history of the solar system. Moreover, surprising differences exist between them, both from a dynamical and a spectroscopic point of view. The objective of this session is to give an outline of the current aspects of the resaearch on KBOs. The session will be organized around the following topics: the dynamical picture of the outer solar system; the taxonomic populations (KBOs, Centaurs, comets); the observational techniques; thermal and structural evolution; surface properties; formation and evolution.
For more information contact:
Maria Teresa Capria
CNR-IASF, Area di Ricerca di Tor Vergata, via del Fosso del Cavaliere, 00133 Rome, Italy
Daisuke Kinoshita (NAOJ) firstname.lastname@example.org
Antonella Barucci (LESIA-Observatoire de Paris) email@example.com
The Division for Planetary Sciences of the American Astronomical Society will hold its 36th Annual Meeting in Louisville, Kentucky November 8-12, 2004. Special features include a Sunday night reception at the Louisville Slugger Museum and a Wednesday night banquet at Churchill Downs, starting with a live race at the historic track. Groundbreaking new science is expected to be announced in Louisville from the recently arrived Cassini Mission to Saturn and Titan, the newly launched Space Infrared Telescope Facility (SIRTF), two recently landed Mars Exploration Rovers (MER), the just-returned Genesis solar-wind sample mission, and more. Local attractions include Fort Knox, Mammoth Cave National Park, Maker's Mark Distillery, My Old Kentucky Home State Park, the Kentucky Horse Park, the Falls of the Ohio State Park, and the new Muhammad Ali Center in downtown Louisville.
Contact information of LOC members is listed at:
The Institute for Astronomy (IfA) invites applications for postdoctoral fellows with a strong interest in astrobiology to collaborate with the University of Hawaii's NASA Astrobiology Institute lead team members. The UH lead team will maintain an innovative multi-disciplinary research environment linking biological, microbiological, chemical, geological and astronomical sciences to investigate the origin, history, distribution and role of water as it relates to life in the universe. The core of this program will center around interactions with an interdisciplinary group of postdoctoral fellows. Areas of primary research collaboration will be:
Minimum qualifications include a Ph.D. and and the expertise appropriate for the specific research focus selected by the applicant. This could include (but is not limited to):
Additional desirable qualifications
The successful candidates will have access to unequaled astronomical observing facilities at the Mauna Kea and Haleakala observatories, an Ultra-High Vacuum Surface scattering machine, a 5 spectrometer electron microprobe and scanning electron microscope, a prototype Cryobot, fully-equipped molecular biology and microbiology laboratories, the R/V Kilo Moana oceanographic research ship, and the University of Hawaii Undersea Research Laboratory. In addition, successful candidates will be in close proximity to a variety of unique aquatic habitats (open ocean, high-altitude lakes, fumaroles). Appointments will be up to 3 years assuming satisfactory progress. Fellows will receive a stipend of $4,333 per mo, a relocation allowance and small research budget. Fellows may apply for an subsequent 2 year position as senior fellows.
Applicants are expected to propose a program of research in
consultation with the lead team members. Please address application
materials including a complete application form (available online at:
includes a CV, publication list, a research proposal describing
connections to at least 2 lead team members (see
http://www.ifa.hawaii.edu/UHNAI) and a list of at least three
professional references to:
Dr. Rolf Kudritzki, Director
Institute for Astronomy
2680 Woodlawn Drive,
Honolulu, HI 96822
Request that the letters of recommendation are sent directly to this same address. Further details may be obtained from Dr. Rolf Kudritzki at 808-956-8566 or email firstname.lastname@example.org. Questions about the UH Astrobiology lead team's program may be directed to Dr. K. J. Meech. Applications will be reviewed beginning Dec. 15, 2003, but the positions will remain open until filled. The University of Hawaii is an EEO/AA employer and encourages applications from women and minorities.
We accept submissions for the following sections:
Distant EKOs is not a refereed publication, but is a tool for furthering communication among people interested in Kuiper belt research. Publication or listing of an article in the Newsletter or the web page does not constitute an endorsement of the article's results or imply validity of its contents. When referencing an article, please reference the original source; Distant EKOs is not a substitute for peer-reviewed journals.