Extreme Solar Systems II – Jackson Lake, 14 September 2011 Stellar Pulsations Excited by Planetary Tides in WASP-33 Andrew Cameron 1, E. Guenther 2, J. M. Matthews 3, J. Telting 8, P. J. Amado 4, I. McDonald 5, E. Shkolnik 6, A. M. S. Smith 7, G. A. H. Walker 9, MOST Science Team 1 University of St Andrews, United Kingdom, 2 Thueringer Landessternwarte Tautenburg, Germany, 3 University of British Columbia, Canada, 4 Instituto de Astrofsica de Andalucia, Spain, 5 Jodrell Bank Centre for Astrophysics, United Kingdom, 6 Carnegie Institution of Washington, 7 Keele University, United Kingdom, 8 Nordic Optical Telescope Scientific Association, Spain, Hewlett Place, Canada.

Extreme Solar Systems II – Jackson Lake, 14 September 2011 H-R diagram for transit-planet hosts Data from F. Pont, HD = WASP-33

Extreme Solar Systems II – Jackson Lake, 14 September 2011 WASP transit detection Transit period = days; R p = 1.53 R jup

Extreme Solar Systems II – Jackson Lake, 14 September 2011 A fast rotator – with pulsations v sin i = 86 km/sec M p < 4 M jup Collier Cameron et al 2010, MNRAS 407, 507

Extreme Solar Systems II – Jackson Lake, 14 September 2011 Doppler shadow of WASP-33b Tautenburg 2008 Oct 18 NOT/Fies 2009 Dec 8 Time Velocity McDonald 2008 Nov 12 Collier Cameron et al 2010, MNRAS 407, 507

Extreme Solar Systems II – Jackson Lake, 14 September 2011 WASP-33 is young 63 Myr 320 Myr 630 Myr 795 Myr 1 Gyr Stellar density = ± solar

Extreme Solar Systems II – Jackson Lake, 14 September 2011  Scuti pulsations in HD15082 Herrero et al A&A 526, L10 (2011)

Extreme Solar Systems II – Jackson Lake, 14 September 2011 WASP-33 and the instability strip Catanzaro et al, MNRAS 411, 1167 (2011)  Scuti pulsators  Dor pulsators HD = WASP-33 OGLE2-TR-L9 HAT-P-6, HAT-P-14 WASP-17

Extreme Solar Systems II – Jackson Lake, 14 September 2011 MOST WASP-33 campaign 2010 De-trended MOST light curve of WASP-33, 2010 October data points 20 planetary orbits

Extreme Solar Systems II – Jackson Lake, 14 September 2011 Coherent pulsations: 20 orbits MOST light curve phase-binned on transit ephemeris f MOST 2f MOST 3f MOST

Extreme Solar Systems II – Jackson Lake, 14 September 2011 Coherent pulsations: 20 orbits MOST spacecraft orbit modulation removed ± c/day f transit

Extreme Solar Systems II – Jackson Lake, 14 September 2011 Resonance or coincidence? Scan hypothetical orbital frequencies fromScan hypothetical orbital frequencies from f trial =12 f orb /13 to 12 f orb /11 f trial =12 f orb /13 to 12 f orb /11 Pick harmonic f = n f trial yielding lowest  2 in range n = 1 … 70.Pick harmonic f = n f trial yielding lowest  2 in range n = 1 … 70. Fraction of trials yieldingFraction of trials yielding  2 <  2 (12 f orb ) = Reject chance alignment with a strong peak, with 98.3% confidence.Reject chance alignment with a strong peak, with 98.3% confidence.  2 (12 f orb ) f orb

Extreme Solar Systems II – Jackson Lake, 14 September 2011 Ground tracks on wave pattern Apparent pattern period: P pattern = m P puls P pattern = m P puls If P pattern ~ P rot and 86 km s –1 < v eq < 200km s –1 then 3 < m < 8 Orbital period: P orb = 12 P puls P orb = 12 P puls How many nodes does the planet’s ground track cross? m=3 4 rotations:1 orbit m=4 3:1 m=5 12:5 m=6 2:1 m=7 12:7 m=8 4:3

Extreme Solar Systems II – Jackson Lake, 14 September 2011 Resonant retrograde ground-tracks m=3,l=6 m=7,l=20m=7,l=10 m=5,l=16 Just right? Too complex? Just right?

Extreme Solar Systems II – Jackson Lake, 14 September 2011 Spectral surf patterns NOT/Fies 2009 Dec 8 m=3,l=6, i=55 o m=7,l=10, i=55 o McDonald 2008 Nov 12

Extreme Solar Systems II – Jackson Lake, 14 September 2011 Conclusions HD15082 = WASP-33 is a hybrid  Sct (Herrero et al 2011) +  Dor pulsatorHD15082 = WASP-33 is a hybrid  Sct (Herrero et al 2011) +  Dor pulsator –Cf. HD (Handler et al. 2002), HD 8801 (Henry & Fekel 2005), BD (MOST; Rowe et al 2006), HD (MOST; King et al 2006), numerous new examples from KEPLER (Balona et al 2011; Catanzaro et al 2001) Strongest pulsation mode (f = 9.84 c/day) resonates with retrograde planet’s orbit:Strongest pulsation mode (f = 9.84 c/day) resonates with retrograde planet’s orbit: P pattern = m P orb / 12 P pattern = m P orb / 12 High-order g-mode excited by planetary tidal bulge passing over nodes of pulsation pattern.High-order g-mode excited by planetary tidal bulge passing over nodes of pulsation pattern. Is extreme stellar surfing a survivable sport for close-in planets?Is extreme stellar surfing a survivable sport for close-in planets?

Extreme Solar Systems II – Jackson Lake, 14 September 2011  Dor +  Sct pulsators  Dor +  Sct pulsators  Dor  Dor – f < 5-10 c/day – high radial order g-modes –convective blocking  Sct  Sct –f > 5 c/day –Low-order radial, nonradial g and p modes – He II ionization opacity Catanzaro et al 2011: KEPLER hybrids