Beaming effect - Harvard-Smithsonian Center for Astrophysics

Beaming effect - Harvard-Smithsonian Center for Astrophysics

BEER algorithm to discover short-period binaries, brown-dwarfs and planets
in CoRoT and Kepler Lightcurves
BEaming, Ellipsoidal & Reflection effects
Simchon Faigler & Tsevi Mazeh
Tel Aviv University
21 September, 1984
Associate Director of the OIR division
• Search for Massive extrasolar planets
• With short orbital periods
2
1985/6:
• Search for Massive extrasolar planets
• With short orbital periods
• Around M stars
• Comparison bright stars 3
Collaboration and Friendship for 27 years
4
5
6
Simchon Faigler Tel Aviv University
Tsevi Mazeh
Tel Aviv University
Dave Latham
Center for Astrophysics
Lars Buchhave University of Copenhagen
Sam Quinn
Center for Astrophysics
Stephane Udry
Observatoire de
Geneva
Damian Segransan
Observatoire de
Geneva
Robert Mathieu
University of Wisconsin
Avi Shporer
CALTECH
- Madison
Shay Zucker
Tel Aviv University
I. Kepler-76b
Simchon Faigler
Lev Tal-Or
Tsevi Mazeh
Dave Latham
Tel Aviv University
Tel Aviv University
Tel Aviv University
Center for
Lars Buchhave
University of
Astrophysics
Copenhagen
II. SuperRotation
Simchon Faigler
Tsevi Mazeh
Tel Aviv University
Tel Aviv University
Leob & Gaudi 2003
10
Beaming effect
4
Fobs
Vr ⎞
⎛ Vr ⎞
⎛
≅ F0 ⎜1 − ⎟ ≅ F0 ⎜1 − 4 ⎟
c ⎠
c ⎠
⎝
⎝
ΔFbeam
Vr
≅4
F
c
BEaming, Ellipsoidal & Reflection
11
Ellipsoidal effect
ΔFellip
F
3
⎛ R1 ⎞ M 2
≅ α ellip ⎜ ⎟
sin 2 i
⎝ a ⎠ M 1
BEaming, Ellipsoidal & Reflection
12
Reflection (and heating) effect
ΔFrefl
F
2
⎛ R ⎞
≅ α refl ⎜ 2 ⎟ sin i
⎝ a ⎠
BEaming, Ellipsoidal & Reflection
13
14
​"↓0 = Time of primary eclipse/transit
​% ​=%−"↓0 ​&↓2' ≈0
15
Beaming
a
−1 / 2
P
−1 / 3
Reflection
a
P
−2
−4 / 3
Ellipsoidal
a
P
−3
−2
16
First Beaming detections – Eclipsing/Transiting systems
P=5.189 d
​"↓()) =9400K
KOI-74
17
Finding non-transiting/non-eclipsing planets/binaries The BEER search challenge
•  Process O(100,000) lightcurves
•  Identify lightcurves with prominent “BEER like”
modulation and extract ​*↓+,- and amplitudes.
•  Prioritize based on data quality and consistency with
a non-luminous companion.
•  Ignore other periodic modulations – star pulsations,
star rotation, RR-Lyr, spots etc.
•  Select O(10) for Radial Velocity follow-up.
18
​"↓0 = Time of minimal Ellipsoidal
& correct Beaming and Reflection signs
​% ​=%−"↓0 ​&↓2' =0
19
Seven new binaries discovered in the Kepler light curves
through the BEER method confirmed by radial-velocity
observations
S. Faigler, T. Mazeh, S. N. Quinn, D. W. Latham, L. Tal-Or
20
I. Kepler-76b
Simchon Faigler
Lev Tal-Or
Tsevi Mazeh
Dave Latham
Tel Aviv University
Tel Aviv University
Tel Aviv University
Center for
Lars Buchhave
University of
Astrophysics
Copenhagen
Kepler-76b: Discovery and confirmation of a hot Jupiter in Kepler data
22
Kepler-76b: Discovery and confirmation of a hot Jupiter in Kepler data
23
Kepler-76b: Discovery and confirmation of a hot Jupiter in Kepler data
S. Faigler, L. Tal-Or, T. Mazeh, D.W. Latham, L. A. Buchhave
24
Kepler-76b: Discovery and confirmation of a hot Jupiter in Kepler data
25
Kepler-76b: Discovery and confirmation of a hot Jupiter in Kepler data
26
?
27
Hot Jupiter Superrotation – HD189733B
Knutson et al. 2007
Knutson et al. 2009
Predicted by Showman & Guillot (2002)
28
II. SuperRotationc
II. Evidence for emission phase shift due to
superrotation in four Kepler hot Jupiters
Simchon Faigler
Tsevi Mazeh
Tel Aviv University
Tel Aviv University
II. SuperRotation
Beaming
Reflection
Ellipsoidal
30
31
II. SuperRotation
Unshifted
BEER model
KOI-13
HAT-P-7
TrES-2
Kepler-76
Unshifted Lambert
reflection
Mp,beam (Mjup)
11.1±1.5
4.1±0.8
1.6±0.2
7.1±1.4
Planet mass from
beaming
Mp,ellip (Mjup)
3.3±0.5
2.0±0.2
1.1±0.2
2.1±0.4
Planet mass from
ellipsoidal
92.1
7.6
4.0
28.2
Χ2 of unshifted null
model χ
2
Shifted Lambert
Reflection
Superrotation
BEER model
Mp,SR
δ SR
(deg)
Ageo
χ
2
P
(Mjup)
3.3±0.5
2.0±0.2
1.0±0.3
2.1±0.4
Planet mass
5.4±0.6
4.1±1.6
37±18
10.2±0.2
Phase-shift angle
0.18±0.01
0.19±0.01
0.018±0.004
0.23±0.02
Geometric albedo
0.02
1.1
0.1
0.2
Χ2 of the model 8E-22
(9.6σ)
1.1E-2
(2.5σ)
4.9E-2
(2.0σ)
1E-7
(5.3σ)
Χ2–test confidence
level
32
33
34