Extreme Solar Systems II – Jackson Lake, 14 September 2011 Stellar Pulsations Excited by Planetary...

Extreme Solar Systems II – Jackson Lake, 14 September 2011

Stellar Pulsations Excited by Stellar Pulsations Excited by Planetary Tides in WASP-33 Planetary Tides in WASP-33

Andrew CameronAndrew Cameron11, E. Guenther, E. Guenther22, , J. M. MatthewsJ. M. Matthews33, J. Telting, J. Telting88, P. J. Amado, P. J. Amado44, , I. McDonaldI. McDonald55, E. Shkolnik, E. Shkolnik66, A. M. S. Smith, A. M. S. Smith77, ,

G. A. H. WalkerG. A. H. Walker99, MOST Science Team , MOST Science Team

11University of St Andrews, United Kingdom, University of St Andrews, United Kingdom, 22Thueringer Thueringer Landessternwarte Tautenburg, Germany, Landessternwarte Tautenburg, Germany, 33University of British University of British

Columbia, Canada, Columbia, Canada, 44Instituto de Astrofsica de Andalucia, Spain, Instituto de Astrofsica de Andalucia, Spain, 55Jodrell Bank Centre for Astrophysics, United Kingdom, Jodrell Bank Centre for Astrophysics, United Kingdom,

66Carnegie Institution of Washington, Carnegie Institution of Washington, 77Keele University, United Keele University, United Kingdom, Kingdom, 88Nordic Optical Telescope Scientific Association, Nordic Optical Telescope Scientific Association,

Spain, Spain, 991234 Hewlett Place, Canada. 1234 Hewlett Place, Canada.


H-R diagram for transit-planet H-R diagram for transit-planet hostshosts

Data from F. Pont, http://www.inscience.ch/transits/

HD 15082 = WASP-33


WASP transit detectionWASP transit detection

Transit period = 1.2199 days; Rp = 1.53 Rjup


A fast rotator – with pulsationsA fast rotator – with pulsations

v sin i = 86 km/sec Mp < 4 M jup

Collier Cameron et al 2010, MNRAS 407, 507


Doppler shadow of WASP-33bDoppler shadow of WASP-33b

Tautenburg 2008 Oct 18

NOT/Fies 2009 Dec 8

Tim

e

Velocity

McDonald 2008 Nov 12

Collier Cameron et al 2010, MNRAS 407, 507


WASP-33 is youngWASP-33 is young

63 Myr

320 Myr

630 Myr

795 Myr

1 Gyr

Stellar density = 0.479 ± 0.007 solar


Scuti pulsations in HD15082Scuti pulsations in HD15082

Herrero et al A&A 526, L10 (2011)


WASP-33 and the instability stripWASP-33 and the instability strip

Catanzaro et al, MNRAS 411, 1167 (2011)

Scuti pulsators

Dor pulsators

HD 15082 = WASP-33

OGLE2-TR-L9

HAT-P-6, HAT-P-14

WASP-17


MOST WASP-33 campaign 2010MOST WASP-33 campaign 2010

De-trended MOST light curve of WASP-33, 2010 October 7 - 31

45615 data points20 planetary orbits


Coherent pulsations: 20 orbitsCoherent pulsations: 20 orbits

MOST light curve phase-binned on transit ephemeris

fMOST

2fMOST

3fMOST

14.228.4

42.6


Coherent pulsations: 20 orbitsCoherent pulsations: 20 orbits

MOST spacecraft orbit modulation removed

9.8444 ± 0.0004 c/day21.071.9 20.54

34.1256.77

12.0077 ftransit


Resonance or coincidence?Resonance or coincidence?

• Scan hypothetical Scan hypothetical orbital frequencies from orbital frequencies from

fftrialtrial =12 =12 f forborb/13 to 12 /13 to 12 fforborb/11/11

• Pick harmonic Pick harmonic ff = = nn fftrialtrial yielding lowest yielding lowest 2 2 in in range range nn = 1 … 70. = 1 … 70.

• Fraction of trials Fraction of trials yielding yielding

22 < < 22(12 (12 fforborb) = 0.017) = 0.017

• Reject chance Reject chance alignment with a strong alignment with a strong peak, with 98.3% peak, with 98.3% confidence.confidence.

2(12 forb)

forb


Ground tracks on wave patternGround tracks on wave pattern

Apparent pattern period: Apparent pattern period:

PPpatternpattern = = mm PPpulspuls

If If PPpatternpattern ~ ~ PProtrot and and

86 km s86 km s–1–1< < vveqeq < 200km s< 200km s–1–1 thenthen 3 < 3 < mm < 8 < 8

Orbital period:Orbital period:

PPorborb = 12 = 12 PPpulspuls

How many nodes does the How many nodes does the planet’s ground track cross?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


Resonant retrograde ground-tracksResonant retrograde ground-tracks

m=3,l=6

m=7,l=20 m=7,l=10

m=5,l=16

Just right? Too complex?

Too complex? Just right?


Spectral surf patternsSpectral surf patterns

NOT/Fies 2009 Dec 8

m=3,l=6, i=55o

m=7,l=10, i=55o

McDonald 2008 Nov 12


ConclusionsConclusions• HD15082 = WASP-33 is a hybrid HD15082 = WASP-33 is a hybrid Sct (Herrero et al Sct (Herrero et al

2011) + 2011) + Dor pulsator Dor pulsator– Cf. Cf. HD 209295 (Handler et al. 2002), HD 8801 (Henry & Fekel HD 209295 (Handler et al. 2002), HD 8801 (Henry & Fekel

2005), 2005), BD+18 4914 (MOST; Rowe et al 2006), HD 114839 (MOST; BD+18 4914 (MOST; Rowe et al 2006), HD 114839 (MOST; King et al 2006), numerous new examples from KEPLER (Balona King et al 2006), numerous new examples from KEPLER (Balona et al 2011; Catanzaro et al 2001) et al 2011; Catanzaro et al 2001)

• Strongest pulsation mode (Strongest pulsation mode (ff = 9.84 c/day) resonates = 9.84 c/day) resonates with retrograde planet’s orbit: with retrograde planet’s orbit:

PPpatternpattern = = m Pm Porborb / 12 / 12

• High-order High-order gg-mode excited by planetary tidal bulge -mode excited by planetary tidal bulge passing over nodes of pulsation pattern.passing over nodes of pulsation pattern.

• Is extreme stellar surfing a survivable sport for Is extreme stellar surfing a survivable sport for close-in planets?close-in planets?


Dor + Dor + Sct pulsators Sct pulsators

• DorDor– f < 5-10 c/dayf < 5-10 c/day

– high radial order high radial order g-modesg-modes

– convective convective blockingblocking

• SctSct– f > 5 c/dayf > 5 c/day

– Low-order radial, Low-order radial, nonradial g and p nonradial g and p modesmodes

– He II ionization He II ionization opacityopacity

Catanzaro et al 2011: KEPLER hybrids

Extreme Solar Systems II – Jackson Lake, 14 September 2011 Stellar Pulsations Excited by Planetary...

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