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Leuven and Nijmegen Universities Asteroseismology Asteroseismology Conny Aerts Universities of Leuven and Nijmegen Material: Springer Monograph, 2010 FAMIAS software package (W. Zima)

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Page 1: Asteroseismology - Astrophysics · Asteroseismology will imply major steps forward in answering these questions. p. 8 Leuven and Nijmegen Universities With your naked eye: 3% of the

Leuven and Nijmegen Universities

AsteroseismologyAsteroseismology

Conny Aerts Universities of Leuven and Nijmegen

Material: Springer Monograph, 2010FAMIAS software package (W. Zima)

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Sir Arthur Stanley Eddington:The Internal Constitution of the Stars

1926

At first sight it would seem At first sight it would seem that the deep interior that the deep interior

of the sun and stars of the sun and stars is less accessible is less accessible

to scientific investigation to scientific investigation than any other region of the than any other region of the

universe.universe.

Sir Arthur Eddington (1882 – 1944)

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Our telescopes may probe Our telescopes may probe farther and farther farther and farther

into the depths of space; into the depths of space; but how can we ever obtain but how can we ever obtain

certain knowledge certain knowledge of that which is hidden of that which is hidden

behind substantial barriers?behind substantial barriers?

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What appliance What appliance can pierce through can pierce through

the outer layers of a star the outer layers of a star and test and test

the conditions within?the conditions within?

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Large variation of internal structureLarge variation of internal structureRed Giant

1 M

•

10 M•

We need to do much better than this !

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Motivation: the crucial rôle of stars Motivation: the crucial rôle of stars

Stars are the sources of the chemical evolution of the Universe:

Massive stars synthesize elements H => Fe Stars with moderate masses form C, N, OChemical evolution strongly dependent on internal mixing processes

Stars are local memory of history of Universe and allow to estimate its age

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Present unknowns in stellar modellingPresent unknowns in stellar modelling

Effect of (differential) internal rotation?Effect of convective overshooting ? => how does mixing occur inside the stars ?Preamble of supernova explosion ?Evolution of close binary systems ?

Asteroseismology will imply major steps forward in answering these questions

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With your naked eye: 3% of the stars is variableHistory History ofof the research topic the research topic

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History of the research topicHistory of the research topicPeriodic largeamplitue variables known since long, e.g. Cepheids, RR Lyraes

Multiperiodicity at low amplitude found in many different kinds of variables

Cause: nonradial oscillations

Idea: every body 'sounds' according to its internal structure => the different oscillation frequencies learn us something about the stellar interior

Between 1900 1990: mainly inventories of variables

Since 1990: use frequency content to derive internal structure parameters

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Introduction into asteroseismologyIntroduction into asteroseismology

aster: starseismos: oscillationlogos: discours, reasoning

Through the analysis of stellar oscillations we want to study the stellar interior

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1dimensional oscillations1dimensional oscillations

Fundamental First overtone Second overtone

nodes

modes

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pressure modespressure modes

More frequent collisions = faster sound speedMore frequent collisions = faster sound speed• Higher temperature = faster sound speedHigher temperature = faster sound speed• Higher density = faster sound speedHigher density = faster sound speed• Lighter gases = faster sound speedLighter gases = faster sound speed

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Why do stars oscillate ?Why do stars oscillate ?Because they have convective outer layers which cause stochastic excitation of oscillations (cf. gong)Because some outer layers act as a heat engine: partial ionisation zones absorb and accumulate energy generated in the stellar interior (opacity mechanism) Forced oscillations may occur due to tidal effects in close binaries

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Pulsating stars are everywherePulsating stars are everywhere

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(l,m) = (3,2) tesseral

(l,m)=(3,3) sectoral

Blue : Moving towards ObserverRed : Moving away from Observer

(l,m)=(3,0) axisymmetric

Characterization of nonradial modes Characterization of nonradial modes

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Internal behaviour of the oscillationsInternal behaviour of the oscillationsThe oscillation pattern at the surface propagates in a continuous way towards the stellar centre.

Study of the surface patterns hence allows to characterize the oscillation throughout the star.

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Theoretical description of oscillationsTheoretical description of oscillations

Perturbation of mass, momentum and energy conservation Solutions ~ exp (2π i t f ) can be found, with f the oscillation frequency of one modeVelocity vector ~ spherical harmonic, consisting of Legendre polynomial with wavenumbers (l,m)Limit of large or small frequency: pressure and gravity modes

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Inversion of the frequenciesInversion of the frequencies

The oscillations are standing sound wavesthat are reflected withina cavity Different oscillationspenetrate to differentdepths and hence probe different layers

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Modes with almost equal frequencyModes with almost equal frequency

Green and yellow oscillations probealmost same region

Such oscillationsallow to map the mixing processeslayer by layer

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Solar frequency spectrum from Solar frequency spectrum from ESA/NASA satellite SoHO: systematics !ESA/NASA satellite SoHO: systematics !

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Musical Intermezzo:Musical Intermezzo: Symphony of the Sun Symphony of the Sun

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Frequencies of a red giant starFrequencies of a red giant star

• VaG22222 Inop de grond, amplitude is 4 keer groter dan bij de zon

• Individuele frequenties zijn niet oplosbaar

1 month RV data of Xi Hya (2002, 1.2m Euler)

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Musical Intermezzo: Musical Intermezzo: Symphony of a red giantSymphony of a red giant

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Frequencies of an sdB starFrequencies of an sdB star

• VaG22222 Inop de grond, amplitude is 4 keer groter dan bij de zon

• Individuele frequenties zijn niet oplosbaar

Qqqq

6 nights of data of PG0014+067 (2004, 4.2m WHT)

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Musical Intermezzo: Musical Intermezzo: Symphony of PG0014+067Symphony of PG0014+067

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Dopplermap of the SunDopplermap of the Sun

The Sun oscillates in thousands of nonradial modes with periods of ~5 minutes

The Dopplermap shows velocities of the order of some cm/s

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The sun as a star BiSONThe sun as a star BiSON

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Frequency separations in the SunFrequency separations in the Sun

Result: internal sound speed and internal rotation could be determined very accurately by means of helioseismic data (SoHO, BiSON, GONG)

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Asteroseismic HR (JCD) diagramAsteroseismic HR (JCD) diagramLarge frequency separation: measure of sound speedSmall frequency separation: measure of discontinuities in the sound speed

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Internal rotation law ?Internal rotation law ?Rotational splitting of the nonradial modes: Needed to solve this set of equations:

Several observed frequency splittings Mode identification (l,m,n)

At present: we are able to treat only slow rotation

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Internal rotation of the SunInternal rotation of the Sun

Beginning of outer convection zone

Solar interior has rigid rotation

X 10¯ Hz9

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But the Sun is just one simple star...But the Sun is just one simple star...

She does not have a large convective coreShe is a slow rotatorShe is relatively unevolved

How do all these results/techniques change for other types of stars ?

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Solarlike Oscillations in Solarlike Oscillations in αα Centauri Centauri

UVES & UCLESUVES & UCLES42 oscillation frequencies42 oscillation frequencies

ℓℓ = 13= 13

Mode lifetimes only Mode lifetimes only 12 days12 days

Noise level = 2 cm sNoise level = 2 cm s11!!

Bedding, T., et al. 2004, ApJ, 614, 380

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Results for Alpha Cen A+B (G2V+K1IV)Results for Alpha Cen A+B (G2V+K1IV)42 & 12 detected frequencies, in range1.8 2.9 & 3.0 4.6 milliHertzAmplitudes between 2 44 & 8 14 cm/sLarge separations = 105.5 & 161.1 micro HzSmall separations = 5.6 & 10.2 micro Hzα CenA has no convective core, although slightly more massive than the Sun (1.105 & 0.934 solar masses)α( Α) < α( Β) by 5 10%Eggenberger et al. (2004); Miglio & Montalban (2004)

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Alpha Cen is more evolved than SunAlpha Cen is more evolved than Sun

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Summary of solarlike oscillatorsSummary of solarlike oscillatorsOscillation frequencies scale as expected

Large (and small) separations derived

Too few frequencies to map interior rotation or tune mixing processesas in the Sun

Need for long-term monitoring of a few selected targets

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Frequency spectra of red giants?Frequency spectra of red giants?

Extensive RV campaigns: Frandsen et al. (2002); De Ridder et al. (2006); Hekker et al. (2006): radial modes or NRP?

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White dwarfs – gmode pulsatorsWhite dwarfs – gmode pulsators

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PG 1159-035

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• TTsurfsurf = 123,000 124,000 K; log g = 123,000 124,000 K; log g ≈≈ 7 7

1000 1000 ≤≤ f f ≤≤ 2600 2600 µµ Hz; 385 Hz; 385 ≤≤ P P ≤≤ 1000 s 1000 s

125 frequencies; >100 modes125 frequencies; >100 modes

M = 0.586 ± 0.003 solar massesM = 0.586 ± 0.003 solar masses

the star is compositionally stratifiedthe star is compositionally stratified

PG 1159035PG 1159035

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BPM 37093BPM 37093DAVDAV

M = 1.09 M = 1.09 MM

TTeffeff = 11730 K = 11730 K

90% crystallized 90% crystallized

CO coreCO core

Metcalfe, T. S.; Montgomery, M. H.; Kanaan, A. 2004, ApJ, 605, 133

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BPM 37093BPM 37093

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Pulsating subdwarf B stars: sdBVPulsating subdwarf B stars: sdBV

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Remarkable discoveries of sdBVsRemarkable discoveries of sdBVs

PG 1336 + 018 (Kilkenny et al. 1998, Vuckovic et al. 2007)

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Remarkable discoveries of sdBVsRemarkable discoveries of sdBVs

Planet survived Red Giant phase of the sdBV starV391 Pegasi... How??

Planet was discoveredin the asteroseismiclightcurve

(Silvotti et al. 2007)

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Loworder p & g modes: Loworder p & g modes: ββ Cephei stars Cephei stars

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Massive star seismology: HD 129929Massive star seismology: HD 129929

Waelkens & Aerts:observed this star during 21 years

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Phase diagrams for U filter dataPhase diagrams for U filter data

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First case study: HD 129929 First case study: HD 129929

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Strategy: forward modellingStrategy: forward modellingDerive set of frequencies & amplitudes from data

Compute stellar models thru error box in HR diagram + predict their unstable oscillation modesX, Z (or Y), M, age (or Teff), core overshoot: 5D

Identify observed modes, either frompattern recognition from theoretical modelsdirect methods (quasiindependent of models)

Confrontation: does the input physics of the models explain the seismic data?

if yes: we get very precise stellar parameters if no: great! Input physics is insufficient and must be upgraded to include additional effects or better descriptions until frequencies can be matched...

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HD129929: Position in HR diagramHD129929: Position in HR diagram

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HD129929: M(Z) relationHD129929: M(Z) relation

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Acceptable range in M,Z,overshootAcceptable range in M,Z,overshoot

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Conclusions for HD129929Conclusions for HD129929

We need very small coreovershooting to explain the frequencies of the star using OPAL opacities and standard solar mixtureFIRST star besides the Sun in which nonrigid rotation is proven: core 3.6 times faster than surface

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Results so far for B starsResults so far for B stars Compatible with EB & isochrone fitting Ref. Star Mass (M) SpT αov (Hp) ΩR(km/s) Ωcore/Ωenv

(1) HD 16582 10.2 ± 0.2 B2IV 0.20±0.10 28(14?) (2) HD 29248 9.2 ± 0.6 B2III 0.10±0.05 6±2 ~5 (3) HD 44743 13.5 ± 0.5 B1III 0.20±0.05 31±5 (4) HD 129929 9.4 ± 0.1 B3V 0.10±0.05 2±1 3.6 (5) HD 157056 8.2 ± 0.3 B2IV 0.44±0.07 29±7 ~1

(1) Aerts et al. (2006): 20 d MOST photometry + 1 week spectra (2) Pamyatnykh et al. (2004); Ausseloos et al. (2004): 5 months multisite photometry + spectroscopy (3) Mazumdar et al. (2006): 4 years highresolution spectroscopy (4) Aerts et al. (2003, 2004); Dupret et al. (2004): 20 years photometry (5) Briquet et al. (2007): 2 years spectroscopy + few months photometry

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Status prior to CoRoT and Kepler Status prior to CoRoT and Kepler Solarlike oscillations in some 30 stars:

Slightly more massive Suns do not have convective coreOscillation frequencies scale as predictedInsufficient frequencies to derive rotational mixingMode lifetimes ?

Discoveries of oscillations in 5 red giants since 2001First proof of nonrigid rotation inside massive stars since 2003: they live longer !Goal: beat the noise level...

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Goal 1: better independent constraintsGoal 1: better independent constraintsProvide an independenthighprecision radius ESOestimate for bright stars VLTICunha et al. (2007, A&ARev)

Provide an independent 2012highprecision distance ESAestimate Gaia

Dedicated instruments Mercatorfor specific stars attached HERMESto private telescopes for MAIAmode identification

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Goal 2: space asteroseismology Goal 2: space asteroseismology MOST: Canadian mission (15cm)launched in June 2003max. 6 weeks, extended

CoRoT: Frenchled European mission (27cm), launched 27/12/2006max 5 months, extended 2013

Kepler : NASA mission (95cm),launch 7 March 2009, exoplanets4 (6?) years

PLATO: exoplanet ESA mission with asteroseismic capabilitiespreselected for CV201520256 years

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What appliance What appliance can pierce through can pierce through

the outer layers of a star the outer layers of a star and test and test

the conditions within?the conditions within?

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