introduction to asteroseismology - vilniaus...
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Introduction to Asteroseismology
Tim Bedding
Sydney Institute for Astronomy,
School of Physics,
University of Sydney
Inside the Sun
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Asteroseismology:
• the study of “starquakes”
• probing stellar interiors using their
oscillations
• What are stellar oscillations?
• Why do stars oscillate?
• How do we observe these oscillations?
• How do we analyse the data?
• What are we learning?
Topics
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Hertzsprung-Russell diagram
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• Many classes of pulsating
stars
• we only discuss solar-like
oscillations
• “pulsation” vs. “oscillation”?
(no difference)
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Convection excites the oscillations by
shaking the star, creating standing waves
Oscillations in the Sun:
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Oscillations in the Sun (Doppler shift)
BiSON (Birmingham Solar
Oscillations Network)
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p-mode oscillations are standing sound waves
n =1 n =3n =2
n is called the radial order of the overtone
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n =18
oscillation frequency of each mode depends on mode
pattern (e.g., n) and on internal sound speed
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Oscillations in the Sun (Doppler shift)
BiSON (Birmingham Solar
Oscillations Network)
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Pow
er
Fourier power spectrum of solar velocities:
p-mode overtones are approximately regularly
spaced in frequency
n increases →
Dn
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n increases →
Centauri A
(Bedding et al. 2004)
the Sun
Centauri B
(Kjeldsen et al. 2005)
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A revolution in
asteroseismology
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figure by Daniel Huber
a few years ago
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CoRoT (27 cm telescope)
Launched: 27 December 2006
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figure by Daniel Huber
red clump
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Kepler95cm Schmidt telescope;. Observations commenced: 1 May 2009
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red clump
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Huber et al. (2011)
red clump
Kepler
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Sun
(SOHO)
KIC 6116048
KIC 6603624
KIC 6106415
KIC 8379927
KIC 8006161
Dn
Dn
Dn Dn
Dn
Dn
Dn
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Sun
(SOHO)
KIC 6116048
KIC 6603624
KIC 6106415
KIC 8379927
KIC 8006161 nmax
nmax
nmaxnmax
nmax
nmax
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Red giants with Kepler (first 30 days)
nmax
nmax
nmax
nmax
nmax
nmax
Brown et al. (1991);
Kjeldsen & Bedding (1995)
Bedding et al. 2010
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Scaling relations:
Solve to get mass and radius:
(and luminosity)
Detailed modelling of individual frequencies gives
much more, including ages
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Huber et al. (2011)
red clump
Kepler
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Chaplin et al. (2011, Science)
• survey of 2000 stars for 1 month each
• detections in 500 stars
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Population studies
(Miglio et al. 2011)
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Miglio et al. (2011)
mass lossOpen clusters
Stello et al. (2011)
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What else can we do?
A closer look at the frequency
spectra...
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n increases →
Centauri A
(Bedding et al. 2004)
the Sun
Centauri B
(Kjeldsen et al. 2005)
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ℓ=2
ℓ=2
2 0
ℓ=0
ℓ=0 ℓ=1
ℓ=1
ℓ=1
Dn = 135 mHz
The Sun
ℓ=3ℓ=33
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ℓ =0 (radial modes)
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ℓ=1 ℓ= 2 ℓ= 3
ℓ =1,2,3,... (non-radial modes)
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• p-mode cavity
in envelope
• g-mode cavity
in core
p mode with l = 2
p mode with l = 0
Christensen-Dalsgaard et al. (lecture notes) and Aerts et al. (2010, “Asteroseismology”)
p modes
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ℓ=2
ℓ=2
2 0
ℓ=0
ℓ=0 ℓ=1
ℓ=1
ℓ=1
Dn = 135 mHz
large separation:
measures mean
density of the star
dn02
ℓ=3ℓ=33
small separations: sensitive to core (age)
dn13
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l = 5
m = 5
l = 10
m = 5
l = 10
m = 10
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Pow
er
Fourier power spectrum of solar velocities:
n increases →
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ℓ=2
ℓ=2
2 0
ℓ=0
n=21,
ℓ=0ℓ=1
ℓ=1
ℓ=1
ℓ=33 ℓ=3
n increases →
Dn = 135 mHz
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http://owww.phys.au.dk/~hans/tidsserie/Lecture_04.pdf
Modes in Sun have
lifetimes of t=2 to 4 days.
Lorenztian envelope:
G=p/t
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The Fabulous Échelle
Diagram
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ℓ=2
ℓ=2
2 0
ℓ=0
ℓ=0 ℓ=1
ℓ=1
ℓ=1
ℓ=33 ℓ=3
Dn = 135 mHz
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Dn=135mHz
Sun
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BISON freq.
The Sun: échelle diagram
l=3l=1
l=0l=2l=0l=2
Frequency mod Dn
Dn
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BISON freq.
The Sun: échelle diagram
l=3l=1
l=0l=2l=0l=2
dn13dn02
Frequency mod Dn
Dn
sensitive to core (age)
measures mean density
(surface effects and acoustic glitches)
curvature
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Exercise 1: make an echelle diagram
with these 14 frequencies
• plot (frequency) versus (frequency mod Dn)
• find the best Dn (hint start with about 120mHz)
• what happens if you change Dn slightly?
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So that is what we are looking for in other stars.
Now for an overview of observational results (some highlights)
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Observations of solar-like
oscillations: some highlights
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Lots of effort in the 1980s, but ...
(written in 1993)
Kjeldsen & Bedding (1995)
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1993: Stars with claimed detections
• e Eridani (K2 V; Noyes et al. 1984)
• Procyon (F5 IV; Gelly et al. 1986; Brown et al. 1991;
. Bedford et al. 1993)
• Cen A (G2 V; Gelly et al. 1986; Pottasch et al. 1992)
• Arcturus (K2 III; Belmonte et al. 1990)
• HD 155543 (F2 V; Belmonte et al. 1990b)
1993: Stars with confirmed detections
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Brown et al. (1991)
Martic et al. (2004)
Eggenberger et al. (2005)
Velocity
observations of
Procyon (F5 IV)
Dn ≈ 55mHz but no agreement on
individual frequencies
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Method 1: changes in velocity
using the Doppler effect
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Method 2: changes in luminosity
(photometry)
why does luminosity change?
answer: surface
temperature changes
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Gilliland et al. (1993)
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1994: h Boo G0 IV (subgiant)
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Method 3: variations in equivalent
widths of temperature-sensitive lines
Hans Kjeldsen
Nordic Optical Telescope,
La Palma
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Kjeldsen et al. (1995)
h Boo: G0 subgiant
confirmation: Kjeldsen et al.
(2003) and Carrier et al. (2005)
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Back to Method 1: what is this?
Planets around the star 47 Ursa Majoris
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2000: b Hyi G2 IV (subgiant, future
Sun)
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Bedding et al. (2001) and Carrier et al. (2001)
UCLESUCLES (Aust.)
CORALIE (Chile)
UCLES at the 3.9m
AAT, Australia
velocities (iodine cell)
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2001: Cen A (G2 V)
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Cen A
Bouchy & Carrier (2001,2002)
CORALIE
CORALIE at the
Swiss 1.2-m
Leonhard Euler
Telescope at La
Silla, Chile
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Butler et al. (2003)
Bedding et al. (2004)
l=1l=2 l=0 l=3
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2007 Back to the future: b Hyi G2 IV
(subgiant, future Sun)
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Bedding et al. (2007)
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2008: The Procyon campaign
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Brown et al. (1991)
Martic et al. (2004)
Eggenberger et al. (2005)
Velocity
observations of
Procyon (F5 IV)
Dn ≈ 55mHz but no agreement on
individual frequencies
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HARPS
CORALIE
McDonald
Lick
UCLES
Okayama
Tautenburg
SOPHIE
EMILIE
SARG
FIES
2008: Velocities of Procyon with a network of
11 telescopes at 8 observatories over 25 days
Arentoft et al. (2008), Bedding et al. (2009)
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Brown et al. (1991)
Martic et al. (2004)
Eggenberger et al. (2005)
Velocity
observations of
Procyon (F5 IV)
Arentoft et al. (2008), Bedding et al. (2009)
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Arentoft et al. (2008), Bedding et al. (2009)
broad modes (short lifetimes)
“bloody F star”
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n Ind (G0 IV metal-poor)
h Boo (G0 IV)
Procyon A (F5 IV)
b Hyi (G2 IV)
m Ara (G3 V)
Cen A (G2 V)
Cen B (K1 V)
t Cet (G8 V)
Examples from
ground-based
spectroscopy
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Ground-based velocity
(stars with reliable Dn)
figure by Dennis Stello
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First node in Tenerife
The next step from the ground: a network dedicated to asteroseismology
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• WIRE (NASA): 5cm
• MOST (Canada): 15cm
• COROT (France/ESA): 27cm
• Kepler (NASA): 95cm
Solar-like oscillations from
space
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Wide Field Infrared Explorer (WIRE)
• launched on 5 March 1999
• primary mission failed
• asteroseismology using the
5cm star camera (Derek
Buzasi)
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WIRE photometry of
red giantsArcturus (Retter et al. 2003)
Stello et al. (2008)
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Launched June 30,
2003 (15 cm)
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more data on Procyon
with MOST: Guenther
et al. (2008)
see also Huber et al.
(2011)
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CoRoT (27 cm)
Launched: 27 December 2006
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F stars with CoRoT
(Michel et al. 2008)
HD 49933
HD 181420
HD 181906
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pre-Kepler
figure by Dennis Stello
●=spectroscopy
○=photometry
Stars with reliable Dn
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HD 49933
Appourchaux et al. (2008),
Benomar et al. (2009), etc.
HD 181420
Barban et al. (2009)
HD 181906
Garcia et al. (2009)
broad modes (short lifetimes)
more bloody F stars
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Red giants with CoRoT
(De Ridder et al. 2009)
beautiful!
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figure by Daniel Huber
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figure by Daniel Huber
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Launched 6 March 2009
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• not in low-Earth orbit
• one field for >4 years
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Saxo
JavaGemma
Sun
http://owww.phys.au.dk/~hans/tidsserie/Lecture_12.pdf
Three G-type stars after one month with Kepler
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Three G stars with Kepler
(Chaplin et al. 2010)
Saxo
Java
Gemma
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Saxo
Java
Gemma
Gilliland et al. (2010)
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Red giants with Kepler (first 30 days)
Bedding et al. 2010
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Exercise 1: make an echelle diagram
with these 14 frequencies
• plot (frequency) versus (frequency mod Dn)
• find the best Dn (hint start with about 120mHz)
• what happens if you change Dn slightly?