Download - Extrasolar Planets and Stellar Oscillations in K Giant Stars Notes can be downloaded from →Teaching
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Extrasolar Planets and Stellar Oscillations in K Giant Stars
Notes can be downloaded from
www.tls-tautenburg.de→Teaching
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20000 14000 10000 7000 5000 3500 2500
1.000.000
10.000
100
1
0.01
0.0001
O B A F G K M
+20
+15
+10
+5
0
-5
-10
Abs
olut
e M
agni
tude
Lum
inos
it y (
Sol
ar L
um. )
Effective Temparature
Spectral Class
White Dwarfs
Main Sequence Giants
Supergiants
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Why the interest in K giants for exoplanets and asteroseismology?
K giants occupy a „messy“ region of the H-R diagram
Progenitors are higher mass stars
Evolved A-F stars
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The story begins:
Smith et al. 1989 found a 1.89 d period in Arcturus
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1989 Walker et al. Found that RV variations are common among K giant stars
These are all IAU radial velocity standard stars !!!
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First, planets around K giants stars…
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1990-1993 Hatzes & Cochran surveyed 12 K giants with precise radial velocity measurements
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Footnote: Period Analysis
Lomb-Scargle Periodogram:
Power is a measure of the statistical significance of that frequency (period):
1
2Px() =
[ Xj sin tj–]2
j
Xj sin2 tj–
[ Xj cos tj–]2
j
Xj cos2 tj–j
+1
2
False alarm probability ≈ 1 – (1–e–P)N = probability that noise can create the signal
N = number of indepedent frequencies ≈ number of data points
tan(2) = sin 2tj)/cos 2tj)j j
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If a signal is present, for less noise (or more data) the power of the Scargle periodogram increases. This is not true with Fourier transform -> power is the related to the amplitude of the signal.
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Many showed RV variations with periods of 200-600 days
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Her has a 613 day period in the RV variations
But what are the variations due to?
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The nature of the long period variations in K giants
Three possible hypothesis:
1. Pulsations (radial or non-radial)
2. Spots (rotational modulation)
3. Sub-stellar companions
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What about radial pulsations?
Pulsation Constant for radial pulsations:
Q = PM
Mּס
( )0.5 R
Rּס
( )–1.5
For the sun:
Period of Fundamental (F) = 63 minutes = 0.033 days (using extrapolated formula for Cepheids)
Q = 0.033
Pּס
( )0.5
=
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Footnote:
The fundamental radial mode is related to the dynamical timescale:
d2R
The dynamical timescale is the time it takes a star to collapse if you turn off gravity
dt2=
GM
R2
Approximate: R ≈ G R is the mean
density
For the sun = 54 minutes
= (G)–0.5
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What about radial pulsations?
K Giant: M ~ 2 Mּס , R ~ 20 Rּס
Period of Fundamental (F) = 2.5 days
Q = 0.039
Period of first harmonic (1H) = 1.8 day
→ Observed periods too long
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What about radial pulsations?
Alternatively, let‘s calculate the change in radius
V = Vo sin (2t/P),
R =2 Vo sin (2t/P) = ∫0
/2 VoP
Gem: P = 590 days, Vo = 40 m/s, R = 9 Rּס
R ≈ 0.9 RּסBrightness ~ R2
m = 0.2 mag, not supported by Hipparcos photometry
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What about non-radial pulsations?
p-mode oscillations, Period < Fundamental mode
Periods should be a few days → not p-modes
g-mode oscillations, Period > Fundamental mode
So why can‘ t these be g-modes?
Hint: Giant stars have a very large, and deep convection zone
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Recall gravity modes and the Brunt–Väisälä Frequency
The buoyancy frequency of an oscillating blob:
N2 = g (1
P
dPdr
–ddr )
g is local acceleration of gravity
is density
P is pressure
Where does this come from?
P
dPd( )
adFirst adiabatic exponent
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Brunt Väisälä Frequency
*
00
T
r
Change in density of surroundings:
= 0 + ( ddr ) r
* = 0 + ( ddP ) r
Change in density due to adiabatic expansion of blob:
dPdr
* = 0 + ( 11
) rdPdr
P
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Brunt Väisälä Frequency
*
00
T
r
Difference in density between blob and surroundings :
= – *
= r( 11
)dPdr
P
ddr
–
Buoyancy force fb = – g r
= –( 1
)ddr
1
1
dP
drP–
F = –kx → 2 = k/mRecall
This is just a harmonic oscillator with 2 = N2
r
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Brunt Väisälä Frequency
Criterion for onset of convection:
However if * < , the blob is less dense than its surroundings, buoyancy force will cause it to continue to rise
( 11
) dPdr
P
ddr
In convection zone buoyancy is a destabilizing force, gravity is unable to act as a restoring force → long period RV variations in K giants cannot be g modes
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What about rotation? Spots can cause RV variations
Radius of K giant ≈ 10 Rּס
Rotation of K giant ≈ 1-2 km/s
Prot ≈ 2R/vrot
Prot ≈ 250–500 days
Its possible!
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Rotation (and pulsations) should be accompanied by other forms of variability
1. Have long lived and coherent RV variations
2. No chromospheric activity variations with RV period
4. No spectral line shape variations with the RV period
3. No photometric variations with the RV period
Planets on the other hand:
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Case Study Gem
CFHT McDonald 2.1m
McDonald 2.7m TLS
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Ca II H & K core emission is a measure of magnetic activity:
Active star
Inactive star
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Ca II emission variations
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Hipparcos Photometry
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Test 2: Bisector velocity
From Gray (homepage)
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Spectral line shape variations
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Period 590.5 ± 0.9 d
RV Amplitude 40.1 ± 1.8 m/s
e 0.01 ± 0.064
a 1.9 AU
Msin i 2.9 MJupiter
The Planet around Gem
M = 1.7 Msun
[Fe/H] = –0.07
The Star
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Frink et al. 2002
P = 1.5 yrs
M = 9 MJ
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P = 711 d
Msini = 8 MJ
Setiawan et al. 2005
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Setiawan et al. 2002:
P = 345 de = 0.68 M sini = 3.7 MJ
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Tau
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Tau has line profile variations, but with the wrong period
Hatzes & Cochran 1998
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Period 653.8 ± 1.1 d
RV Amplitude 133 ± 11 m/s
e 0.02 ± 0.08
a 2.0
Msin i 10.6 MJupiter
The Planet around Tau
M = 2.5 Msun
[Fe/H] = –0.34
The Star
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Dra
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Period 712 ± 2.3 d
RV Amplitude 134 ± 9.9 m/s
e 0.27 ± 0.05
a 2.4
Msin i 13 MJupiter
The Planet around Dra?
M = 2.9 Msun
[Fe/H] = –0.14
The Star
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Setiawan et al. 2005
The evidence supports that the long period RV variations in many K giants are due to planets…so what?
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B1I V
F0 V
G2 V
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Planets around massive K giant stars
Dra 2.9 13 2.4 712 0.27 –0.14
Tau 2.5 10.6 2.0 654 0.02 –0.34
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Period
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Characteristics:
1. Supermassive planets: 3-11 MJupiter
Theory: More massive stars have more massive disks
2. Many are metal poor
Theory: Massive disks can form planets in spite of low metallicity
3. Orbital radii ≈ 2 AU
Theory: Planets in metal poor disks do not migrate because they take so long to form.
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And now for the stellar oscillations…
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Hatzes & Cochran 1994
Short period variations in Arcturus
n = 1 (1H)
n = 0 (F)
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n
0 F1 1H2 2H
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Ari
Alias
n≈3 overtone radial mode
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Dra
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Dra : June 1992
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Dra : June 2005
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Dra
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Photometry of a UMa with WIRE guide camera (Buzasi et al. 2000)
0
1
23
Radial modes n =
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Conclusion: most (all?) K giant stars pulsate in the radial and low-overtone modes.
So what?
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HD 13189
P = 471 d
Msini = 14 MJ
M* = 3.5 s.m.
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P = 4.8 days
P = 2.4 days
HD 13189 short period variations
For M = 3.5 Mּס
R = 38 R
F = 4.8 d
2H = 2.7 d
→ oscillations can be used to get the stellar mass
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Current work on K giants
1. TLS survey of 62 K giants (Döllinger Ph.D.)
2. Multi-site campaigns planned (GLONET)
3. MOST campaign on Oph and Gem
4. CoRoT additional science program (150 days of photometry)
5. Lots of theoretical work to model pulsations needs to be done
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Döllinger Ph.D. work: 62 K giants surveyed from TLS
≈ 10% show long period variations that may be due to planetary companions
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Time (days)
Inte
nsit
y5.7 days
Aldebaran with MOST
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Summary
• K giant (IAU radial velocity standards) are RV variable stars!
• Multi-periodic on two time scales: 200-600 days and 0.25 – 8 days
• Long period variations are most likely due to giant planets around stars with Mstar > 1 Mּס
• Short period variations are due to radial pulsations in the fundamental and overtone modes
• Pulsations can be used to get funamental parameters of star