- ID:
- ivo://CDS.VizieR/J/AJ/156/33
- Title:
- Resonance sticking in the population of scattering TNOs
- Short Name:
- J/AJ/156/33
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A substantial fraction of our solar system's trans-Neptunian objects (TNOs) are in mean-motion resonance with Neptune. Many of these objects were likely caught into resonances by planetary migration-either smooth or stochastic- approximately 4 Gyr ago. Some, however, gravitationally scattered off of Neptune and became transiently stuck in more recent events. Here we use numerical simulations to predict the number of transiently stuck objects, captured from the current actively scattering population, that occupy 111 resonances at semimajor axes a=30-100 au. Our source population is an observationally constrained model of the currently scattering TNOs. We predict that, integrated across all resonances at these distances, the current transient-sticking population comprises 40% of the total transiently stuck+scattering TNOs, suggesting that these objects should be treated as a single population. We compute the relative distribution of transiently stuck objects across all p:q resonances with 1/6=<q/p=<1, p<40, and q<20, providing predictions for the population of transient objects with H_r_<8.66 in each resonance. We find that the relative populations are approximately proportional to each resonance's libration period and confirm that the importance of transient sticking increases with semimajor axis in the studied range. We calculate the expected distribution of libration amplitudes for stuck objects and demonstrate that observational constraints indicate that both the total number and the amplitude distribution of 5:2 resonant TNOs are inconsistent with a population dominated by transient sticking from the current scattering disk. The 5:2 resonance hence poses a challenge for leading theories of Kuiper Belt sculpting.
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- ID:
- ivo://CDS.VizieR/J/AJ/127/3023
- Title:
- R magnitudes of Kuiper Belt object 2001QG298
- Short Name:
- J/AJ/127/3023
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Extensive time-resolved observations of Kuiper belt object 2001 QG298 show a light curve with a peak-to-peak variation of 1.14+/-0.04mag and single-peaked period of 6.8872+/-0.0002hr. The mean absolute magnitude is 6.85mag, which corresponds to a mean effective radius of 122(77)km if an albedo of 0.04(0.10) is assumed. This is the first known Kuiper belt object and only the third minor planet with a radius greater than 25km to display a light curve with a range in excess of 1mag. We find the colors to be typical for a Kuiper belt object (B-V=1.00+/-0.04, V-R=0.60+/-0.02), with no variation in color between minimum and maximum light.
- ID:
- ivo://CDS.VizieR/J/A+A/569/A3
- Title:
- Rotational properties of TNOs
- Short Name:
- J/A+A/569/A3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results for the short-term variability of Binary Trans-Neptunian Objects (BTNOs). We performed CCD photometric observations using the 3.58m Telescopio Nazionale Galileo (TNG), the 1.5m Sierra Nevada Observatory (OSN) telescope, and the 1.23m Centro Astronomico Hispano Aleman (CAHA) telescope at Calar Alto Observatory. We present results based on five years of observations and report the short-term variability of six BTNOs. Our sample contains three classical objects: (174567) 2003 MW_12_, or Varda, (120347) 2004 SB_60_, or Salacia, and 2002 VT_130_; one detached disk object: (229762) 2007 UK_126_; and two resonant objects: (341520) 2007 TY_430_ and (38628) 2000 EB_173_, or Huya. For each target, possible rotational periods and/or photometric amplitudes are reported. We also derived some physical properties from their lightcurves, such as density, primary and secondary sizes, and albedo. We compiled and analyzed a vast lightcurve database for Trans-Neptunian Objects (TNOs) including centaurs to determine the lightcurve amplitude and spin frequency distributions for the binary and non-binary populations. The mean rotational periods, from the Maxwellian fits to the frequency distributions, are 8.63+/-0.52h for the entire sample, 8.37+/-0.58h for the sample without the binary population, and 10.11+/-1.19h for the binary population alone. Because the centaurs are collisionally more evolved, their rotational periods might not be so primordial. We computed a mean rotational period, from the Maxwellian fit, of 8.86+/-0.58h for the sample without the centaur population, and of 8.64+/-0.67h considering a sample without the binary and the centaur populations. According to this analysis, regular TNOs spin faster than binaries, which is compatible with the tidal interaction of the binaries. Finally, we examined possible formation models for several systems studied in this work and by our team in previous papers.
- ID:
- ivo://CDS.VizieR/J/A+A/407/1139
- Title:
- RVB photometry of Kuiper-Belt object 1999 TD10
- Short Name:
- J/A+A/407/1139
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present photometric observations of the Kuiper-Belt object 1999 TD_10_ at different phase angles and for three different broad band filters (B, V and R). This object was observed with the Danish 1.54-m telescope of ESO in Chile during six different observing nights corresponding to a phase angle of 0.30, 0.37, 0.92, 3.43, 3.48 and 3.66{deg}. Extra observations were obtained in September 2002 with the VLT UT1/FORS1 combination to confirm that 1999 TD_10_ does not exhibit any cometary activity, and in October 2001 with the Sierra Nevada Observatory 1.50-m telescope in order to add relative magnitudes to improve the determination of the rotation period.
- ID:
- ivo://CDS.VizieR/J/A+A/610/A2
- Title:
- Saturnian satellites Cassini ISS astrometry
- Short Name:
- J/A+A/610/A2
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Caviar is a software package designed for the astrometric measurement of natural satellite positions in images taken using the Imaging Science Subsystem (ISS) of the Cassini spacecraft. We provide new astrometric positions for selected major satellites of Saturn, 2013-2016.
- ID:
- ivo://CDS.VizieR/J/A+A/572/A43
- Title:
- Saturnian satellites Cassini ISS astrometry
- Short Name:
- J/A+A/572/A43
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We provide astrometric observations of the Saturnian satellites Mimas, Enceladus, Tethys, Dione and Rhea from Cassini Imaging Science Subsystem (ISS) narrow-angle camera (NAC) images. Image sequences were designed to observe mutual occultations between these satellites.
- ID:
- ivo://CDS.VizieR/J/A+A/645/A76
- Title:
- Saturnian satellites in the Gaia ref. frame
- Short Name:
- J/A+A/645/A76
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a remeasurement of old photographic plates, providing important raw data for dynamical studies of the Saturnian satellite system. The unprecedentedly accurate realization of the Gaia reference frame allows us to make a precise calibration of digitized astronegatives of the Saturnian satellite images. We reprocessed 357 astronegatives taken with the 26-inch refractor and the normal astrograph of the Pulkovo Observatory between 1972 and 2007 to obtain the positions of the main Saturnian moons in the second Gaia data release (Gaia DR2) system. Photographic plates were digitized with the Pulkovo Mobile Digitizing Device (MDD) scanner. The New Astrometric Reduction of Old Observations (NAROO) digitizer at the Paris Observatory was used to calibrate the scanned images. Satellite image centering and astrometric reduction were performed. In total, 6487 positions (equatorial coordinates) have been determined with an accuracy of 50mas. This is confirmed by a comparison of our data with modern ephemerides. The verification of the results was performed using data from past close approaches by Saturnian satellites to Gaia reference stars, showing the adequacy of the current residual analysis. A joint review of the Pulkovo and the United States Naval Observatory (USNO) intersatellite positions allows us to conclude about the existence of faint systematic effects in the satellite theories of motions at the 10mas level.
- ID:
- ivo://CDS.VizieR/J/A+A/383/296
- Title:
- Saturnian Satellites positions (1996-2000)
- Short Name:
- J/A+A/383/296
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- 199 frames of CCD images of the major satellites of Saturn (Mimas, Enceladus, Tethys, Dione, Rhea, Titan, Hyperion and Iapetus), obtained on 1-meter telescope at the Yunnan Observatory during the years of 1996-2000, are measured. These positions are compared to the ones computed with the Vienne & Duriez ephemerides (TASS1.7). The calibrated parameters of the CCD scale and orientation are determined by the comparison of their measurement coordinates with computed positions of four bright satellites of Tethy, Dione, Rhea and Titan. A catalog of 913 differential positions has been obtained. Analysis of the data as inter-satellite positions shows that these observations of the above mentioned four satellites have root-mean-square residuals of 0.04 arcsec in the sense of (O-C) (Observed minus Computed). The positional measuring procedure is proved to be good enough to obtain a small dispersion in the observations for the major Saturn satellites. The format of the present catalog are very near to the one of (Strugnell & Taylor, 1990A&AS...83..289S). The coordinates are corrected by all astrometric effects. So, these positions are really astrometric ones in that meaning that, no astrometric consideration is necessary to use them, even if one wants to touch up the calibration. Nevertheless, the raw pixels are also given in order to allow anyone to reduce again the frames.
- ID:
- ivo://CDS.VizieR/J/AJ/159/129
- Title:
- 21 saturnian small moons brightness with ISS
- Short Name:
- J/AJ/159/129
- Date:
- 08 Dec 2021
- Publisher:
- CDS
- Description:
- We examine the surface brightnesses of Saturn's smaller satellites using a photometric model that explicitly accounts for their elongated shapes and thus facilitates comparisons among different moons. Analyses of Cassini imaging data with this model reveal that the moons Aegaeon, Methone, and Pallene are darker than one would expect given trends previously observed among the nearby mid-sized satellites. On the other hand, the trojan moons Calypso and Helene have substantially brighter surfaces than their co-orbital companions Tethys and Dione. These observations are inconsistent with the moons's surface brightnesses being entirely controlled by the local flux of E-ring particles, and therefore strongly imply that other phenomena are affecting their surface properties. The darkness of Aegaeon, Methone, and Pallene is correlated with the fluxes of high-energy protons, implying that high-energy radiation is responsible for darkening these small moons. Meanwhile, Prometheus and Pandora appear to be brightened by their interactions with the nearby dusty F-ring, implying that enhanced dust fluxes are most likely responsible for Calypso's and Helene's excess brightness. However, there are no obvious structures in the E-ring that would preferentially brighten these two moons, so there must either be something subtle in the E-ring particles's orbital properties that leads to asymmetries in the relevant fluxes, or something happened recently to temporarily increase these moons's brightnesses.
- ID:
- ivo://CDS.VizieR/J/A+A/621/A113
- Title:
- Saturn lightning episodes of storm F
- Short Name:
- J/A+A/621/A113
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The paper analyzes a lightning storm on Saturn that raged for 7.5 months at a planetocentric latitude of 35 deg. south from 27 November 2007 until 15 July 2008. The storm system produced about 277000 lightning events termed SEDs (for Saturn Electrostatic Discharges) that were detected by the Cassini RPWS (Radio and Plasma Wave Science) instrument. The SEDs are organized in episodes, lasting typically for half a Saturn rotation. SEDs can be detected when the observer Cassini is within the radio horizon (usually when the storm and Cassini are on the same side of the planet), and they are not detected when Cassini is beyond the radio horizon (Cassini and the storm on opposite sides). Saturn's atmospheric storm features have a much higher angular velocity than Cassini around Saturn, so that one SED episode is typically related to one Saturn rotation. The SEDs from this storm, lasting from the end of Nov. 2007 until mid-July 2008 (termed storm F), occurred in 439 SED episodes.
