The Rossiter- McLaughlin Effect

Transcription

1 The Rossiter- McLaughlin Effect B. Scott Gaudi The Ohio State University (special thanks to Josh Winn)

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3 Relative flux Time

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21 Gaudi & Winn (2007)

22 What is the Rossiter-McLaughlin Effect?

23 What do we measure?

24 What do we measure? K O V(t) = V O (t) +V R (t) +V 0 Doppler V O (t) = K O {cos[ f (t) +!]+ ecos!} " K = 2!G % O $ ' # P & 1/3 msini (M + m) 2/3 (1( e2 ) (1/2

25 What do we measure? K O V(t) = V O (t) +V R (t) +V 0 Anomalous RV

26 What exactly is the RM effect? Change in line shape Not a Doppler shift Cross-correlation measures line centroids Some methods attempt to correct for line shape variations

27 y x V(x, y) = xv * sin I Centroid approximation V R = V * sin I V R = V * sin I!!!! xs(x, y)dxdy S(x, y)dxdy! = r R! 2 1"! 2 g(t; x p, y p,!,u 1,...) # K R g(t) Ohta et al 2005 Gimenez 2006

28 No limb-darkening, complete transit V R = K R g(t) g(t) = x(t) =! cos" # bsin " where! = t " t tra T! b! 2 K R = V * sin I 1"! 2 ~ K R t rot! t tra T ~ b tan"

29 Measuring spin-orbit alignment Ohta, Taruya, & Suto 2005; Gaudi & Winn 2007

30 Parameters Specified by the photometric transit: Duration Ingress/Egress Time Impact Parameter Limb Darkening Planet/Star Radius Ratio Additional Parameters Required for RM Effect λ (Spin-Orbit alignment) V * sini (can also be constrained from spectrum)

31 Total S/N S N! Q R $ 1 (1" 4b2 )cos 2 # + b 2 1/2 & % 3 ' where Q R = N! K R S N! 50

32 Measurement Uncertainties % $1 (1$ b 2 )cos 2 " + 3b 2 sin 2 " (! " # Q R ' * & b 2 (1$ b 2 ) )! V* sin I V * sin I " Q % #1 (1# b 2 )sin 2 $ + 3b 2 cos 2 $ ( ' * R & b 2 (1# b 2 ) ) 1/2 1/2 Gaudi & Winn (2007) Useful for estimating expected uncertainties

33 Central Transits are bad:! V R = K R (! cos" # bsin ") $ [K R cos"]! λ is degenerate with V * sini

34 Why Measure the Rossiter-McLaughlin Effect?

35 Spin-orbit alignment for exoplanets

36 Spin-orbit alignment for exoplanets Solar system: alignment is within ~10 o

37 Spin-orbit alignment for exoplanets Solar system: alignment is within ~10 o How common or unusual is this?

38 Spin-orbit alignment for exoplanets Solar system: alignment is within ~10 o How common or unusual is this? Theoretical reasons to expect misalignment:

39 Spin-orbit alignment for exoplanets Solar system: alignment is within ~10 o How common or unusual is this? Theoretical reasons to expect misalignment: Whatever perturbs e may also perturb I

40 Spin-orbit alignment for exoplanets Solar system: alignment is within ~10 o How common or unusual is this? Theoretical reasons to expect misalignment: Whatever perturbs e may also perturb I Migration (disk interaction v. scattering, Kozai)

41 Planet-Planet Scattering Chatterjee, Ford, & Rasio (2007)

42 Kozai Oscillations with Tides Fabrycky &Tremaine (2007) Wu et al (2007)

43 Kozai Oscillations with Tides

44 Spin-orbit alignment for exoplanets Solar system: alignment is within ~10 o How common or unusual is this? Theoretical reasons to expect misalignment: Whatever perturbs e may also perturb I Migration (disk interaction v. scattering, Kozai) Fundamental measurement

45 Measurements of the Rossiter-McLaughlin Effect

46 R. A. Rossiter ( )

47 β Lyrae: Rossiter 1924, ApJ, 60, 15 R. A. Rossiter ( )

48 β Lyrae: Rossiter 1924, ApJ, 60, 15 Algol: McLaughlin 1924, ApJ, 60, 22 R. A. Rossiter ( )

49 Queloz et al 2000

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52 Ω star i star ψ λ Ω orbit λ = / 1.4 deg (RM effect) Winn, Holman, Henry, et al. (2007) sin i star = [v sin i star ] / (2πR/P ) ψ < 27 deg (95% conf.)

53 HD = HAT-P-2 Bakos et al. (2007) Diagram by G. Laughlin

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55 TrES-1: λ= 30º ±21º (Narita et al 2007) HD : λ= 12º ±14º (Wolf et al)

56 Spin-orbit alignment for exoplanets

57 Spin-orbit alignment for exoplanets Random alignments ruled out (>99.9% CL)

58 Spin-orbit alignment for exoplanets Random alignments ruled out (>99.9% CL) Tidal coplanarization takes too long

59 Spin-orbit alignment for exoplanets Random alignments ruled out (>99.9% CL) Tidal coplanarization takes too long Hut 1981; Queloz et al. 2000; Winn et al. 2005

60 Spin-orbit alignment for exoplanets Random alignments ruled out (>99.9% CL) Tidal coplanarization takes too long Hut 1981; Queloz et al. 2000; Winn et al Migration generally preserves spin-orbit alignment?

61 Confirming Planets Rossiter-McLaughlin Effect

62 RM Effect Amplitude K R K O! # P & % ( $ 2"Gm ' "! 0.3 $ # m M Jup 1/3 % ' & V * sin I (1/3 " P % $ ' # 3 days& 1/3 " V sin I % $ * ' # 5 km/s & Doppler and RM amplitude of the same order for Hot Jupiters Larger for less massive planets, or longer period planets

63 Earthlike Planet Gaudi & Winn (2007) Welsh et al (2004)

64 Confirming Kepler Detections Gaudi & Winn (2007)