9807

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

@MISC{2014ktwo.propGO6025,
	author = {{Ryan}, R. and {Woodward}, W.},
	title = {Lightcurves of Trojan and Hilda asteroids: Insight into the formation of planetesimals},
	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 and Trojan
		 asteroids populations yield key information about the primordia
		l shape and binary fraction of these small body populations. Mil
		li-mag Kepler photometry will tightly constrain both of the latt
		er characteristics. These two populations are in stable resonanc
		es with Jupiter (Hildas in the 3:2 resonance at 4 AU, Trojans ar
		e located at 5 AU in the L4 and L5 Lagrange points of the Sun-Ju
		piter system) and collisional frequencies within these populatio
		ns are the lowest within inner solar system small body populatio
		ns [8-9]. Results from the WISE survey suggest that ~20% of Troj
		an asteroids and ~40% of Hilda asteroids are either extremely el
		ongated objects, or are binaries[10]. Kepler optical light curve
		s are required to confirm these controversial findings. Ground b
		ased optical surveys are not optimal for this type of photometri
		c variability survey. Large amounts of observing time are requir
		ed, and analysis of lightcurves obtained over a few nights is ha
		mpered by aliasing induced by limited photometric sampling over 
		regularly spaced nightly intervals. Kepler however is ideal for 
		this type of photometric survey of asteroid variability due to t
		he photometric stability of the observing platform and the corre
		spondence between the Campaign 6 field and the L4 Trojan cloud.W
		e have identified ~120 objects for study in the Hilda and Trojan
		 asteroid populations to be studied with Kepler in Campaigns 6 &
		amp; 7 with magnitudes of m_V < 20.  Due to the overlap betwe
		en the Campaign 6 field and the L4 Trojan cloud, our request for
		 data represents 110 objects Campaign 6 and 10 objects in Campai
		gn 7. These objects are not stationary within the Kepler fields,
		 rather they move across the field, resulting in a mean time in 
		the Kepler field of view on active silicon of 24 days for our ta
		rgets. We will utilize data obtained with the 30 minute Kepler c
		adence to determine rotational periods for our selected targets.
		 The ratio of lightcurve amplitudes will subsequently be utilize
		d to determine body elongation and/or binarity to test the resul
		ts reported by the WISE survey.}
	howpublished = {K2 Proposal},
	year = {2014},
	month = {October},
	url = {https://keplerscience.arc.nasa.gov/data/k2-programs/GO6025.txt},
	notes = {K2 Proposal GO6025}
}

                    Acknowledgement:
                    This work uses...