617 patroclus and menoetius - carmenes.caha.escarmenes.caha.es/cab/sol/2013-2014/oppenheimer.pdf ·...
TRANSCRIPT
617 Patroclus and MenoetiusA Binary Minor Planet
Outline
1. Introduction
2. Patroclus and Menoetius1. Detection and parameters
2. Composition
3. Orbital angular momentum
3. Conclusion and Outlook
Patroclus a Trojan Asteroid
• The Trojans are in the astronomieasteroids around the Lagrangianpoints L4 and L5 of Jupiter
• They are named after the warriors ofthe trojan war and sperated in thetwo camps
• Two exceptions: Patroclus and Hector who were discovered before theconfession and are therefore in theoposite Lagrangian point
Discovery of Patroclus
• Patroclus was discovered on the 17th of October in 1906 by Kopff, A. at Heidelberg
• It was the secound trojan asteroid discovered after Hector
• It has a diameter of 122±3 km and the mass of the total system is 1.36 ± 0.11 × 1018 kg and therefore a density of 0.88 ± 0.17
𝑔𝑐𝑚3
• It has a absolute magnitude of 8.19 mag
Discovery of Menoetius
• Menoetius was discovered on 22nd of September in 2001 from: William J. Merline, Laird M. Close, N. Siegler, D. Potter, Clark R. Chapman, Christophe Dumas, François Menard und David C. Slater
• It was discovered with the 8.1 meter-Gemini-North-Telescope in Hawaii
• With a diameter of 112.6 ± 3.2 km it is about 7% smaller than Patroclus
The binary system parameters
Period (days) 4.283 ± 0.004
Semi-major axis (km) 680 ± 20
Eccentricity, e 0.02 ± 0.02
Orbit pole solution ECJ2000 (λ and β in degrees)
λ = 236 ± 5, β = -61 ± 1
Pericentre argument (degrees) 139
Time of passage (Julian days, JD) 2453171.1 ± 0.1
Total mass (kg) (1.36 × 1018) ± 0.11
Bulk density of the system* (g 𝑐𝑚−3) 0.8± 0.17 𝑔 𝑐𝑚3
The orbital angular momentum
• The origin of this tightly bound, small-eccentricity and large angular-momentum binary system remains unclear
• Could be the reuslt of a capture, with subsequent circularization ofthe orbit by tidal effects
• Other explination could be a low velocity impact of large projectile(less probable)
• Could also be formed by tidal effects after low-velocity encounterwith large planet
• Spin periods of components unknown
• Probable a unsynchronized system
Composition of the Asteroids
• Similiar distant to Sun like Galileansatallites → mixture of ice and androck (≜ 50% porosity )
• With the low density of 0.88 ± 0.17
𝑔𝑐𝑚3 it is quite probable that they
consist of water/ice (≜ 15%porosity).
• Referring to Dynimical simulations itis possible that they were formed in the outer solars system
Conclusion and Outlook
• Formation unclear
• Simulations show that several distant planetesimals have a close approach with Jupiter before their final capture at the Lagrange points
• a special programme of photometric observations should be undertaken to attempt to derive the spin poles and rates.
Thank you for your attention!