Dynamics of the WASP-3 system

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