CCD photometric observations of seven asteroids were obtained from the Center for Solar System Studies from 2016 April to June.
CCD photometric observations of seven asteroids were obtained from the Center for Solar System Studies from 2016 April to June.
Analysis of CCD photometric observations of the near-Earth asteroid (331471) 1984 QY1 show that it is likely in non-principal axis rotation (NPAR), or tumbling. A single period analysis found a dominant period of 45.5 ± 0.5 h, but the true periods of rotation and precession could not be determined.
The very wide binary asteroids (VWBA) are a subgroup of binary asteroids that exhibit very long primary periods and, mostly, short secondary periods that are similar to those of the primary of "normal" small binary asteroids. It is unlikely that confirming mutual events will be seen by photometric observations, mostly because the orbital periods of the assumed satellites will be on the order of days. This paper introduces three additional candidates for this subgroup: (215442) 2002 MQ3, 2009 EC, and 2016 BU13. All three are considered to be among the more convincing examples that such systems exist.
Analysis of CCD photometric observations of near-Earth asteroid (154244) 2002 KL6 indicate that it may be a binary system. The presumed primary has a synodic rotation period of 4.60869 ± 0.00005 h and lightcurve amplitude of 0.65 ± 0.03 mag. The presumed satellite has an orbital period of 24.05 ± 0.02 h and maximum lightcurve amplitude of 0.07 mag. The secondary lightcurve showed no mutual events and seems to indicate that the satellite's rotation is tidally locked to its orbital period.
We present lists of asteroid photometry opportunities for objects reaching a favorable apparition and have no or poorly-defined lightcurve parameters. Additional data on these objects will help with shape and spin axis modeling via lightcurve inversion. We also include lists of objects that will be the target of radar observations. Lightcurves for these objects can help constrain pole solutions and/or remove rotation period ambiguities that might not come from using radar data alone.
CCD photometric observations in 2016 February and March and a reevaluation of observations made in 2013 June of 19204 Joshuatree show it to be a possible binary. It is another candidate for the special case of very wide binaries. The primary lightcurve has a period of 480 ± 5 h and an amplitude 0.25 ± 0.02 mag. and the secondary lightcurve has a period of 21.25 ± 0.05 h.
Lightcurves for 16 main-belt asteroids were obtained at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2015 December into 2016 April.
Lightcurves for 38 near-Earth asteroids (NEAs) were obtained at the Center for Solar System Studies-Palmer Divide Station (CS3-PDS) from 2016 January-April. Also reported are 4 lightcurves obtained from 2014-2015 that were not previously published.
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