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Global Helioseismology NSO/LPL Summer School June 11-15, 2007 [email protected]

Global Helioseismology NSO/LPL Summer School June 11-15, 2007 [email protected]

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Page 1: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Global Helioseismology

NSO/LPL Summer School

June 11-15, 2007

[email protected]

Page 2: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

History

• Discovered in 1960 that the solar surface is rising and falling with a 5-minute period

• Many theories of wave physics postulated:– Gravity waves or acoustic

waves or MHD waves?– Where was the region of

propagation?• A puzzle – every attempt to

measure the characteristic wavelength on the surface gave a different answer

Page 3: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

The puzzle solved

• Acoustic waves trapped within the internal temperature gradient predicted a specific dispersion relation between frequency and wavelength

• A wide range of wavelengths are possible, so every early measurement was correct – result depended on aperture size

• Observationally confirmed in 1975

• 5,000,000 modes, max amplitude 20 cm/s

Page 4: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Three types of modes

• G(ravity) Modes – restoring force is buoyancy – internal gravity waves

• P(ressure) Modes – restoring force is pressure

• F(undamental) Modes – restoring force is buoyancy modified by density interface – surface gravity waves

Page 5: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Wave trapping• G modes exist where ω < N2 (Brunt-Väisälä frequency)

• P modes exist where ω < ωac (acoustic cut-off frequency) and ω > S (Lamb frequency)

• F modes are analogous to surface water waves

Page 6: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

The essential frequencies

Page 7: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Frequency units

• ν = 1/(Period in seconds), units are Hertz (Hz)

• ω = 2π/(Period in seconds), units are radians/sec

• P = 5 min = 300 sec, ν = 3.33 mHz or 3333.33 μHz; ω = 2.1 10-2 rad/s

Page 8: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Acoustic-Gravity Waves

Unstratified Stratified

Page 9: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Ray Paths

Turning points

QuickTime™ and aYUV420 codec decompressor

are needed to see this picture.

QuickTime™ and aYUV420 codec decompressor

are needed to see this picture.

Page 10: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu
Page 11: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Turning points

Page 12: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Quantization

Vertical quantization:

Horizontal quantization:

Modes must live long enough to travel around circumference and self-interfere. Average interior sound speed is 70-100 km/s, thus requires lifetime longer than 0.5 days (Q > 20000).

Page 13: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Spherical Harmonics

n – radial order: 0 n 80

– spherical harmonic degree: 0 4000

m – azimuthal degree: - m

Page 14: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Duvall law• Modes turn at depth

where sound speed = horizontal phase speed = ν/ℓ

• So, all modes with same ν/ℓ must take same time to make one trip between reflections

Page 15: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Rotational Splitting

• In absence of rotation, have standing wave pattern and degenerate case – the frequency 0 ( = /2) is independent of m

• In presence of rotation, prograde and retrograde waves have different

• Observed frequency = m δ where δ is the splitting frequency

• Exactly analogous to a spinning bell

Page 16: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Observing Time Series

X

X

X

=

=

=

Σ QuickTime™ and aYUV420 codec decompressor

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Page 17: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

An Observational Problem

• The sun sets at a single terrestrial site, producing periodic time series gaps

• The solar acoustic spectrum is convolved with the temporal window spectrum, contaminating solar spectrum with many spurious peaks

Page 18: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Solutions

• Antarctica – max 6 month duration

• Network – BiSON, IRIS, GONG – needs data merging, but maintainable

• Space – SoHO+MDI, GOLF – no merging but fragile.

Page 19: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Modern experiments

GONG SOHO

Page 20: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Observing & processing challenges

• Image geometry is paramount

• Image scale affects ℓ-scale

• Angular orientation mixes m-states

• Fitting of spectral features not trivial

• Can only view portion of solar surface, so have spatial leakage

Page 21: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Solar Acoustic Spectra

- Diagram

m- Diagram-m- Diagram

Page 22: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu
Page 23: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu
Page 24: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu
Page 25: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Inversions 1

Page 26: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu
Page 27: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Eigenfunctions & Kernels

• G Modes – in the core, not observed (but maybe…)

• P Modes – throughout entire sun, but primarily in convection zone

• F Modes – at the surface

• Inversion kernels constructed from eigenfunctions weighted by density

Page 28: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Resolution kernels

• Trade-off between depth resolution and error magnification

• Trade-off curve

Res kernels

Trade-off curve

Page 29: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Internal Rotation

Tachocline

Near-surface shear layer

Page 30: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Temporal Evolution of Zonal Flows

Page 31: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Temporal Evolution

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Page 32: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Tachocline oscillation

Fig. 2 shows the rotation residual in the tachocline, and Fig. 3 shows the power spectrum over different periods. Panels a and d are in the ascending and descending phases of cycle 23, respectively, and show a dramatic difference in the character of the variation. Will this be repeated in cycle 24?

Rachel Howe

Page 33: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

G modes?Simulation

Observation

Analysis uses:

• very long time series (10 years) to take advantage of phase coherency

• even period spacing of g modes

• assumed internal rotation

• estimated observational SNR

Intriguing, but needs verificationGarcia et al, Science, June 15, 2007

Page 34: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Oscillations and the Solar Activity Cycle

• As the activity increases:– The frequencies

increase

– The energy decreases

– The lifetimes decrease

• All of these changes are associated with the surface magnetic field

Page 35: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Oscillations & magnetic field

Mode width (1/lifetime)

Energy

Page 36: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Constraining solar structure

& models• Neutrino experiment

solved• All exotic models

inconsistent with measured frequencies

• Standard model pretty good, but still discrepancy below CZ

• Near surface poorly understood

Page 37: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Sound Speed Variations

Magnetic field?

Thermal perturbations?

Page 38: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Observed-computed frequencies

Page 39: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Sound Source - Granulation

Generates a randomly excited field of damped Helmholtz oscillators

QuickTime™ and aYUV420 codec decompressor

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Page 40: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Excitation Puzzles

Line asymmetry V-I frequency offset

Page 41: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Acoustic Emission Lines

Page 42: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

The sun as a star

• Low-degrees (ℓ = 0, 1, 2, 3)• Large and small separations

– Large: frequency separation between ℓ and ℓ + 1– Small: frequency separation between ℓ and ℓ + 2

• Echelle diagrams– Cut spectrum into 136 μHz segments and stack

• Core rotation• Asteroseismology

Page 43: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Separations

Page 44: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Echelle diagram

Page 45: Global Helioseismology NSO/LPL Summer School June 11-15, 2007 fhill@noao.edu

Next topic

• Local Helioseismology