Echoes of earlier controversies: Hayden Planetarium in New York created a bit
of a stir by omitting Pluto from its list of planets
Reported in IAU Circular 7583
http://cfa-www.harvard.edu/iauc/07500/07583.html): Tony Farnham of
U. Texas detected a 0.5-mag amplitude visible lightcurve in 2000 WR106. The
single-peak period is about 3 hours.
As mentioned last month, 2000 WR106 has the honor of being the object that has gone from discovery to being eligible for numbering in the shortest amount of time (about one month, thanks to detections on historical plates). Not only has it been given one of the ``thousands'' numbers (20000) but is has also been named: Varuna. So to add yet another superlative upon the heap, this is the first TNO to be named. Not being familiar with the name, here's what I dug up as a short bio: Varuna is from pre-Vedic Hindu mythology, and was viewed as a lord of the cosmos, keeper of divine order, and bringer of rain. He is the master of oceans and rivers, and is the deity of fluidity and movement.
There were 2 new TNO discoveries announced since publication of the previous issue of the Distant EKOs Newsletter:
2000 YW134, 2001 CZ31
and 1 new Centaur/SDO discovery:
2000 GV146 (TNO SDO)
2000 GY146 (TNO SDO)
2000 YC2 (TNO SDO)
1999 CG119 (SDO TNO)
Objects with recently assigned numbers and names:
2000 WR106: (20000) Varuna
1995 QZ9: (20108)
1996 TR66: (20161)
Current number of TNOs: 366 (and Pluto & Charon)
Current number of Centaurs/SDOs: 67
Using the Max-Planck Millimeter Bolometer Array (MAMBO) at the IRAM 30m telescope we detected emission at 250 GHz from the Centaur Chariklo (1997 CU26). The observed continuum flux density implies a photometric diameter of 273 km. The resulting geometric albedo is 0.055, somewhat higher than expected from a comparison with most of the other few Centaurs and cometary nuclei for which such data are available.
Published in: Astronomy & Astrophysics, 366, L9 (2001 February)
For preprints, contact firstname.lastname@example.org
We describe the discovery circumstances and photometric properties of 2000 EB173, now one of the brightest trans-Neptunian object with opposition magnitude mR=18.9 and also one of the largest Plutinos, found with the drift-scanning camera of the QUEST Collaboration, attached to the 1-m Schmidt telescope of the National Observatory of Venezuela. Shortward of 0.7 microns, we measure and , a red color observed for many fainter TNOs. At longer wavelengths we measure a relatively neutral color , a color transition previously observed only for a few fainter TNOs. At our magnitude limit , our single detection reveals a sky density of 0.015+0.034-0.012 TNOs per square degree (the error bars are confidence limits), consistent with fainter surveys, showing a cumulative number proportional to . Assuming an inclination distribution of TNOs with FWHM exceeding 30 degrees, it is likely that there are one to several hundred objects brighter than mR=20.1 that remain to be discovered.
Published in: The Astrophysical Journal Letters, 548, L243, (2001 February 20)
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or on the web at
We develop a general method of determining the unbiased inclination distribution of the Kuiper belt using only the inclination and latitude-of-discovery of known Kuiper belt objects (KBOs). These two parameters are well determined for each discovered object, so we can use all 379 known KBOs (as of 1 January 2001) - without knowing the object's precise orbit, or the area, detection efficiency or latitudinal coverage of the survey which found the object - to determine the inclination distribution. We find that a natural analytic form for the inclination distribution is a sine of the inclination times a gaussian. The inclination distribution of all KBOs is well fit by times a sum of two gaussians with widths 2.6+.8-.2 and degrees. For this inclination distribution, the Kuiper belt has an effective area of 8100+1500-1100 square degrees and a FWHM of degrees in latitude. The inclination distribution of the different dynamical classes appear different. The plutinos are well fit by times a single gaussian of width 10.2+2.5-1.8 degrees, the classical KBOs canno t be fit to a single gaussian but are well fit by times the sum of two gaussians of widths 2.2+.2-.6 and degrees, and the scattered KBOs are poorly fit by times a single gaussian of width degrees. The poor fit of the scattered objects is possibly a result of limitations of the method in dealing with large eccentricities.
The effective areas of the plutinos, classical KBOs, and scattered KBOs are , , and square degrees, respectively. The FWHMs are , 6.8+2.0-3.6, and degrees. In all cases, the inclinations of the Kuiper belt objects appear larger than expected from dynamical simulations of possible perturbations.
To appear in: The Astronomical Journal
Preprints on the web at
Dynamic autoresonance theory is applied to the problem of thresholds on migration timescales for capture into resonances in the planar-restricted three-body problem with and slowly migrating masses m1,2. The thresholds are found analytically, scale as (m2 / m1)-4/3, and yield an order of magnitude longer timescales required for capture of m0 into 2:1 outer resonance as compared with 3:2 and other resonances. The difference is due to the rotation of the primary mass m1, affecting the 2:1 resonance only. This could explain the observed small abundance of Kuiper Belt objects in the 2:1 resonance and could define accurate bounds on the timescales involved in the early evolution of the solar system.
Published in: The Astrophysical Journal, 547, L75 (2001 January 20)
Three resonances, the 3:2 mean motion resonance, the Kozai resonance, and the 1:1 superresonance, are known to govern the stability of the motion of Pluto concurrently. In this work, we report an extensive numerical exploration of the 1:1 superresonance region in element space and the effects of the giant planets on this resonance. It is shown that the 1:1 superresonance region is narrower than those for the other two resonances and that it is a second-order resonance. We use the orbits of known Plutinos to investigate our result. None of these Plutinos is in the 1:1 superresonance. We also find that the Jovian planets, especially Jupiter, play important roles in concert in the superresonance.
Published in: The Astronomical Journal, 121, 1155 (2001 February)
For preprints, contact firstname.lastname@example.org
The consistent increase in the discovery rate of new asteroids and Trans Neptunian Objects (TNOs) in these last years has urged an update of the values of intrinsic probability of collision and impact velocity for some minor body populations. With the statistical method of Dell'Oro & Paolicchi (1998), we have recomputed the values of impact probability and velocity for Hilda asteroids, for Trojans vs. Short Period Comets (SPC), and for TNOs. The algorithm of Dell'Oro and Paolicchi is particularly suited for the task since it can account for resonant behaviour (Dell'Oro et al. 1998) and for the clustering of the perihelion longitude of Main Belt asteroids and Hildas, caused by the presence of a forced component in the eccentricity. The Hilda population turns out to be well sampled in the orbital parameter space since no significant changes are found for the collision frequency among Hildas, and of Hildas with Main Belt asteroids, although a much larger sample of orbits has been used in our computations (232 objects) vs. the smaller group used in previous computation by Dahlgren (1998) (40 objects). We also computed the impact rate of SPCs vs. Trojans that turned out to be an order of magnitude lower respect to the Trojans vs. Trojans impact rate. The relative velocity is instead about 30% higher. Using reasonable estimates of SPC and Trojan number densities, we find that approximately 1 every 100 collisions involving Trojans may be with an SPC. In the case of TNOs there is a consistent discrepancy between our values of the collision probability and impact speed, and those computed by Davis & Farinella (1997). The consistent increase in the number of known TNOs (186 at present, only 16 at the time of the Davis and Farinella's work) has led to a better knowledge of their distribution in the phase space and, consequently, to more reliable estimates of the collisional probability and impact velocity.
Published in: Astronomy & Astrophysics, 366, 1053 (2001 February)
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Pluto and its satellite Charon regularly occulted or transited each other's disks from 1985 through 1990. The light curves resulting from these events (collectively called ``mutual events'') have been used to determine albedo maps of Pluto's sub-Charon hemisphere. We now use a data set of four light curves that were obtained in both B and V Johnson filters to construct a two-color map of Pluto's surface. We are able to resolve the central part of Pluto's sub-Charon hemisphere. We find that the dark albedo feature that forms a band below Pluto's equator is comprised of several distinct color units. We detect ratios of V-filter/B-filter normal reflectances ranging from 1.15 to 1.39 on Pluto's sub-Charon hemisphere.
Published in: The Astronomical Journal, 121, 552 (2001 January)
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or on the web at
We used the near-infrared camera and multiobject spectrometer NICMOS on the Hubble Space Telescope to obtain 1.1-2.4 m, low-resolution ( ) slitless grism spectrophotometry of the individual members of the Pluto-Charon system. Water ice is present in its crystalline state on both the leading and trailing hemispheres of Charon. A 2.21 m absorption band, possibly due to the presence of ammonia hydrate in surface, is detected in the reflectance spectrum of its leading side only. Geological activity on Charon or implantation of ions escaped from Pluto's atmosphere could account for the formation of species such as NHH2O locally on the satellite. We also measured a slightly higher geometric albedo for Charon than reported from the mid-1980s observations of the mutual events.
Published in: The Astronomical Journal, 121, 1163 (2001 February)
For reprints, contact Christophe.Dumas@jpl.nasa.gov
or on the web at
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