the solar interior and helioseismologysp2rc.group.shef.ac.uk/assssp16/lectures/l06chaplin.pdfthe...
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The Solar Interior
and
Helioseismology
Bill Chaplin, School of Physics & Astronomy University of Birmingham, UK
STFC Advanced Summer School, 2016 Sep 6
University of Sheffield
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http://solarscience.msfc.nasa.gov/predict.shtml
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http://solarscience.msfc.nasa.gov/predict.shtml
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http://solarscience.msfc.nasa.gov/predict.shtml
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http://solarscience.msfc.nasa.gov/predict.shtml
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http://solarscience.msfc.nasa.gov/predict.shtml
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http://solarscience.msfc.nasa.gov/predict.shtml
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Seismology as a
probe of the
solar cycle Bill Chaplin, School of Physics & Astronomy
University of Birmingham, UK
STFC Advanced Summer School, 2016 Sep 6
University of Sheffield
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Four solar cycles with BiSON
Chaplin & Basu, Space Science Reviews,
2014, 186, 437
23 22 21 24
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Acoustic signatures of the solar
cycle: where it all started…
SMM/ACRIM data
Woodard & Noyes 1985, Nature; 1988, IAU123
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Clear correlations with surface
measures of activity
Elsworth et al. 1990, Nature, 345, 322
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Frequency dependence
at low degree
Elsworth et al. 1994, ApJ, 434, 801
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Frequency and degree dependence
of shifts…
Libbrecht & Woodard 1990, Nature, 345, 779
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Sound waves generated at top of
Convection Zone...
Convection Zone
Radiative Interior
Photosphere
Acoustic source
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The Resonant Sun The Sun resonates like a musical instrument...
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Standing acoustic wave
patterns...
Internal acoustic
ray paths
Surface displacement:
spherical harmonics
red waves give…
blue waves give…
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Project onto spherical harmonics
l: number of
nodal lines
m: number of
azimuthal
nodal lines
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Internal Solar Rotation
GONG data
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The Tachocline (‘speed slope’)
Courtesy P. H. Scherrer, SOI Stanford
Located just
beneath base of
convection zone
Key for dynamo
action!
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The Solar Activity Cycle
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Resonance in simple 1-D pipes
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Directly, by action of Lorentz force
Indirectly by changing stratification
Changes in Mode Properties...
Magnetic fields can act as
agents of change:
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Effects of near-surface activity on modes Depends on spherical harmonic of mode (l, m)
(1,0) (1,1) (2,0)
(3,0) (2,2) (2,1)
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Effects of near-surface activity on modes Depends on spherical harmonic of mode (l, m)
(3,1) (3,2) (3,3)
(10,10) (10,5) (5,5)
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Global Frequency Shifts in GONG
data: as Function of Solar Latitude
Courtesy R. Howe
Spatial dependence
correlates strongly
with active regions
Dependence of
shifts on mode
degree, l, and mode
frequency, suggests
near-surface effect
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Variations in Global
Mode Damping and
Energy
La
titu
de
1996 1997 1998 1999 2000 2001 1996 1997 1998 1999 2000 2001
60
20
-20
-60
Energy (forcing/damping) Mode Damping
Komm, Howe & Hill, 2002
Inference on changes to
convection, which excites
and damps modes
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Torsional oscillations of
the whole convection
zone
Difference in
successive 72-d
rotation inversions of
MDI data
Courtesy S. Vorontsov and collaborators
Migrating bands of flow penetrate interior!
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Slow start to cycle 24
Howe et al. (2013)
Near-surface flows: GONG, MDI, HMI
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Dynamics: comparing solar minima
Antia & Basu (2010)
MDI & GONG data: cycle 24 – cycle 23
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Tachocline oscillations
Howe et al. 2011, JPCS
GONG and MDI data
Above
tachocline
Beneath
tachocline
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Structure: comparing solar minima
BiSON frequencies: cycle 24 – cycle 23
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“Sounding” stellar activity cycles: Sun BiSON Sun-as-a-star data
scaled 10.7-cm radio flux
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Broomhall et al., 2012, ApJ, 420, 1405
Quasi-biennial
variation
After removal of
11-yr cycle
signature
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Cycles 22, 23… and rise of 24 BiSON Sun-as-a-star data
High-frequency
modes
Intermediate-frequency
modes
Low-frequency
modes
scaled 10.7-cm radio flux scaled ISN
22 23 24
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Standing acoustic wave
patterns...
Internal acoustic
ray paths
Surface displacement:
spherical harmonics
red waves give…
blue waves give…
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MMdVME nlV
nl /ξ2
1
22
2
1
2
1nlnlnlnl vMEvM
Frequency dependence of shifts
Mode inertia and mode mass
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Frequency dependence
of shifts
Chaplin et al. 2001, MNRAS, 324, 910
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Chaplin et al. 2001, MNRAS, 324, 910
Frequency dependence of shifts
)(/ nlnlnl EEQ
: inertia an l=0 mode would have at frequency nl )( nlE
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Frequency dependence of shifts
UTP for radial modes (model ‘S’)
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nl
nlnl
E
)(
Frequency dependence of shifts
nl
nl
)(
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Chaplin et al. 2001, MNRAS, 324, 910
11)]3000(/[
EEnlnl
Frequency dependence of shifts
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What do we expect for ?
Change confined close to surface
(but in the interior): = 0
Change confined to photosphere
(within one pressure scale height): = 3
Frequency dependence of shifts
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Chaplin et al. 2001, MNRAS, 324, 910
0 2
Frequency dependence of shifts
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Cycles 22, 23… and rise of 24 BiSON Sun-as-a-star data
High-frequency
modes
Intermediate-frequency
modes
Low-frequency
modes
scaled 10.7-cm radio flux scaled ISN
22 23 24
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And now the fall of Cycle 24…
High-frequency
modes
Intermediate-frequency
modes
Low-frequency
modes
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Kepler and CoRoT Exquisite quality photometric data
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Surface temperature (degrees Kelvin)
Lum
inosity ( S
un)
Asteroseismology
of solar-type stars
and red giants
CoRoT
More than 1,000 red giants
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Surface temperature (degrees Kelvin)
Lum
inosity ( S
un)
Approx. 700 solar-type stars
Approx.16,000 red giants
Over 100 planet-hosting stars
Asteroseismology
of solar-like
oscillators
Kepler
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Nielsen et al., 2013, A&A, 568, L12
Rotation of main-sequence stars l=2,0 and 1 modes in Kepler target KIC 6106415
2
0 1
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Chaplin et al., 2013, ApJ, 766, 101
Rotation of main-sequence stars Dipole modes in two Kepler planet hosting stars
Kepler-50 Kepler-65
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Internal rotation of a subgiant Core rotates five-times faster than surface
Deheuvels et al., 2012, ApJ, 756, 19
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Internal rotation from Kepler
Deheuvels et al., 2014, A&A, 564, 27
envelopes
cores
/2 (
nH
z)
log g (dex) Teff (K)
(
Hz)
sub-giants and low-luminosity red giants
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Convection
zone depth
Mazumdar et al., 2014, ApJ
From “acoustic glitches”
Kepler example:
solar-type dwarf
Signal present in
particular combinations
of frequencies
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Signatures of stellar activity Kepler lightcurves of solar-type stars
Basri et al., 2011, ApJL, 713, 155
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Surface rotation periods Kepler lightcurves of solar-type stars
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Stellar cycles with Kepler? From variability of lightcurve: two F-type stars
Mathur et al., 2014, A&A, 562, 124
Time (days)
Time (days)
F
/F (
ppm
)
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The Sun amongst stars
Gilliland, Chaplin et al., 2015, AJ, 150, 133
Kepler stars
Sun
Selection of solar-type stars (Kepler) and
the Sun (SOHO/VIRGO)
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Age-rotation comparisons
Garcia et al. 2014
A&A, 572, 34
Davies et al.
2014, MNRAS
446, 2959
do Nascimento
Jr. et al. 2014,
ApJ, 790, L23
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CoRoT reveals a short activity
cycle in HD49933
García et al., 2010, Science, 329, 1032
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Kepler: solar-type stars with
3+ years of asteroseismic data
Kepler Objects of Interest
KASC field stars
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Asteroseismic inference on
distribution of near-surface activity
(1,0) (1,1) (2,0)
(3,0) (2,2) (2,1)
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Inference: surface distribution of activity sizes and phases of frequency shifts depend on (l, m)
Chaplin (2011), Proceedings Tenerife Winter School
Sun-as-a-star data
max=40 ± 10 degrees
Chaplin et al. 2007, MNRAS, 377, 17
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End