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Proposal Identification No.:

R3036 Arecibo Observatory

Date Received: 2015-Aug-31 14:44:08 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Sep 1 2015. This proposal has not been submitted before. Proposal Type: General Category: Observation Category: Time Requested this semester: Hours already used for this pro ject: Additional Hours required to complete pro ject: Minimum Useful Time: Expected Data Storage: Prop osal Title: Regular Planetary Radar Solar System 21

2h less than 100 GB

Observations of a near-Earth asteroid (85990) 1999 JV6 with Arecibo Planetary

Radar
ABSTRACT: Radar observations are an excellent source of information about the sizes, spin-states and shapes of near-Earth asteroids. We propose to use the Planetary Radar for observations of a small near-Earth asteroid (85990) 1999 JV6 during a close approach in January 2016. The target is selected from the YORP-detection candidates monitored optically with the ESO Large Programme led by S. C. Lowry and has been already observed at Arecibo in January 2015. The proposed observations will be complemented by existing optical photometric lightcurve data, covering the period between 2007 and 2015. Linking the radar observations with the photometric data will help to refine its shape and spin-state model allowing determination of the strength of YORP torques on this body. Outreach Abstract: In this pro ject we will use the Arecibo radar to take images of the asteroid 1999 JV6 and make a 3-D model of its shape. The shape of the asteroid will be used in connection with data from optical telescopes to investigate the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect. The YORP effect is caused by sunlight interacting with an asymmetrically shaped asteroid. It can change the rate at which an asteroid spins. The study of YORP effect helps us understand how asteroids are shaped by forces other than gravity and can give us insight into their internal structure. As an asteroid spins, the amount of sunlight reflected off its surface and reaching the observer changes. We can see this as a repeating change in brightness. We use the asteroid shape models to simulate those changes, called the rotational lightcurves. With a radar-derived shape model and many lightcurves even small changes in rotation rate of 1999 JV6 can be precisely measured.

Name Agata B Rozek Michael C Nolan

Institution University of Kent University of Arizona

E-mail ar377@kent.ac.uk nolan@naic.edu

Phone

Student G no

1


Additional Authors
Stephen C. Lowry, University of Kent, S.C.Lowry@kent.ac.uk

This work is part of a PhD thesis.

Remote Observing Request

X

Observer will travel to AO Remote Observing In Absentia (instructions to operator)

Section I I - Time Request
The following times are in AST. For these observations night-time is required.

Begin ­ End Interval­Interval ­ ­ ­ ­

Days Needed at This Interval

Time Constraints (Must Be Justified in the Prop osal Text) See Proposal text for detailed time request

Section I I I - Instruments Needed
S-Band radar S-band receiver

Atmospheric Observation Instruments:

Sp ecial Equipment or setup:

none

Section IV - RFI Considerations
2


Frequency Ranges Planned
2370-2390

Section V - Observing List Target List
Asteroid 1999 JV6

3