2000 DV76

@ARTICLE{asteriks,
               author = {{Hedges}, C. and Co},
                title = "{}",
              journal = {},
            archivePrefix = "arXiv",
               eprint = {},
             primaryClass = "",
             keywords = {},
                 year = ,
                month = ,
               volume = ,
                pages = {},
                  doi = {},
               adsurl = {},
            }

@MISC{2015ktwo.propGO10010,
	author = {{Ryan}, R. and {Woodward}, W.},
	title = {Lightcurves of  Hilda asteroids: Tracing migrations in the early solar system},
	abstract = {Studies of the small bodies of the solar system reveal important
		 clues about the condensation and formation of planetesimal bodi
		es, and ultimately planets in planetary systems. Dynamics of sma
		ll bodies have been utilized to model giant planet migration wit
		hin our solar system [1-5], colors have been used to explore com
		positional gradients within the protoplanetary disk [6-7], and s
		tudies of the size-frequency distribution of main belt asteroids
		 may reveal compositional dependences on planetesimal strength w
		hich may limit models of planetary growth from collisional aggre
		gration of planetesimals. Studies of the optical lightcurves of 
		asteroids also yield important information on shape and potentia
		l binarity of asteroidal bodies.Light curves of Hilda asteroids 
		populations yield key information about the primordial shape and
		 binary fraction of these small body populations. Milli-mag Kepl
		er photometry will tightly constrain both of the latter characte
		ristics. This population is in the stable 3:2 resonance with Jup
		iter at 4 AU and collisional frequencies within these population
		s are the lowest within inner solar system small body population
		s [8-9]. Results from the WISE survey suggest that  ~40% of Hild
		a asteroids are either extremely elongated objects, or are binar
		ies[10]. Kepler optical light curves are required to confirm the
		se controversial findings. Ground based optical surveys are not 
		optimal for this type of photometric variability survey. Large a
		mounts of observing time are required, and analysis of lightcurv
		es obtained over a few nights is hampered by aliasing induced by
		 limited photometric sampling over regularly spaced nightly inte
		rvals. Kepler however is ideal for this type of photometric surv
		ey of asteroid variability due to the photometric stability of t
		he observing platform.We have identified ~12 objects for study i
		n the Hilda asteroid populations to be studied with Kepler in Ca
		mpaigns 8 & 10 with magnitudes of m_V < 20. These objects
		 are not stationary within the Kepler fields, rather they move a
		cross the field, resulting in a mean time in the Kepler field of
		 view on active silicon of 40 days for our targets. We will util
		ize data obtained with the 30 minute Kepler cadence to determine
		 rotational periods for our selected targets. The ratio of light
		curve amplitudes will subsequently be utilized to determine body
		 elongation and/or binarity to test the results reported by the 
		WISE survey.}
	howpublished = {K2 Proposal},
	year = {2015},
	month = {June},
	url = {https://keplerscience.arc.nasa.gov/data/k2-programs/GO10010.txt},
	notes = {K2 Proposal GO10010}
}

                    Acknowledgement:
                    This work uses...