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Dynamica l S tab i l i t y o f the WASP-3 Sys tem
Florian FreistetterBarbara Funk, Elke Pilat-Lohinger, Richard Schwarz
HCM8, Bad Hofgastein22. March 2011
YET I
Young Exoplanet Transit Initative
YET I
Gunma/Japan: Hidenori TakahashiLulin/Taiwan: Wen-Ping Chen Seline Chia-Ling HuXinglong/China: Zhen-Yu Wu,Zhou XuByurakan/Armenia: Hayk Harutyunyan Tigran MovessianRohzen/Bulgaria: Dinko Dimitrov Diana KjurkchievaStara Lesna/Slovak Rep.: Theo Pribulla Jano Budaj, Martin VankoTorun/Poland: Gracjan Maciejewski Andrzej NiedzielskiRostock/Germany: Ronald Redmer Nadine Nettelmann Ulrike Kramm
Jena/Germany: Ralph Neuhäuser, Ronny Errmann, Stefanie Rätz, Markus Mugrauer, Florian FreistetterMunich/Germany: Johannes KoppenhoeferGranada/Spain: Matilde FernandezArmazones/Chile: Rolf Chini, Vera HoffmeisterCIDA/Venezuela: Cesar BricenoCfA Harvard/USA: Willie TorresStony Brook/USA: Fred WalterSwathmore/USA: Erin Jensen, David CohenGettysburg/USA: Larry MarschallBig Bear Obs/USA: Aglae Kellerer
WASP-3
WASP-3: F7V star with 1.24 Msun
Planet, found in 2007: M=2.06 Mjup a=0.0317 AU e=0
→ Variations in the Transit time?
WASP-3
MNRAS
New observations of WASP-3b Transits
WASP-3
O-C Diagram
litertature data
new data
WASP-3
additional planet?
15MEarth
at 0.0507 AU
(close to 2:1 resonance)
additional family of solutions close to 5:3 res
Observa t ions vs . S imu la t ions Observations can not give exact orbits
Additional source of information to
constrain observations or the possibility
of additional objects
→ Dynamics
Can numerical simulations help?
47 UmaHD 4208
Stab i l i t y D iagram
Stab i l i t y D iagram:chang ing e_p l
e_pl=0.05
e_pl=0.1
Eccentricity of Wasp-3b has tobe small
How eccentric can WASp-3b be?
Stab i l i t y D iagram:chang ing inc l ina t ion
Region of instability dissolves
i=10° i=20°
i=30°
Stab i l i t y D iagram:chang ing mass and eccen t r i c i t y
M=1.93 MJ M=2.19 MJ
e=0.00
e=0.05
e=0.10
Stab i l i t y D iagram:chang ing tes t pa r t i c le mass
no big difference between 1, 7 and 15Earthmasses
M=1 MEarth M=7 MEarth
M=15 MEarth
Cons t ra in ts?
Dynamical constraints on the eccentricity and mass of WASP-3b
better constraints on WASP-3c → more observations → analysis of resonances
WASP-3c lies inside the stable region → but very close to the chaotic region
Trans i t - T ime Var ia t ions
Resonances enhance TTVs
2:1 res (0.0503AU) 0.0507AU
away from res 0.0507AU, e=0.1
Trans i t - T ime Var ia t ions
2:1 res (0.0503AU) 3:2 res (0.0415AU)
2:1 has larger stable region for low e
Trans i t - T ime Var ia t ions
5:2 res (0.0584AU) 5:3 res (0.0446AU)
5:2 stable for low e; 5:3 unstable
Conc lus ions
published values of WASP3c can lead to stable orbits WASP3c lies very close to chaotic region 2:1 resonance is a better place for a planet than 5:3 or 3:2
new observational campaigns are currently ongoing → new data will lead to new parameters of WASP3c → new dynamical constraints
T H EE N D
