The Real Music of the Spheres

Slides:



Advertisements
Similar presentations
Dr. Annie Baglin, COROT Principal Investigator, CNES.
Advertisements

1 A B Models and frequencies for frequencies for α Cen α Cen & Josefina Montalbán & Andrea Miglio Institut d’Astrophysique et de Géophysique de Liège Belgian.
Constraints and Measurements of the Equation of State from the White Dwarf Stars Don Winget Department of Astronomy and McDonald Observatory University.
Extreme Solar Systems II – Jackson Lake, 14 September 2011 Stellar Pulsations Excited by Planetary Tides in WASP-33 Andrew Cameron 1, E. Guenther 2, J.
The Group of Bootis Stars Dr. Ernst Paunzen Institute for Astronomy University of Vienna.
Solar-like Oscillations in Red Giant Stars Olga Moreira BAG.
Asteroseismology of solar-type stars Revolutionizing the study of solar-type stars Hans Kjeldsen, Aarhus University.
A ground-based velocity campaign on Procyon Tim Bedding (Univ. Sydney) and about 50 others.
SEARCHING FOR PLANETS IN THE HABITABLE ZONE. FROM COROT TO PLATO Ennio Poretti – INAF OAB.
Observational properties of pulsating subdwarf B stars. Mike Reed Missouri State University With help from many, including Andrzej Baran, Staszek Zola,
Reaching the 1% accuracy level on stellar mass and radius determinations from asteroseismology Valerie Van Grootel (University of Liege) S. Charpinet (IRAP.
Exoplanet- Asteroseismology Synergies Bill Chaplin, School of Physics & Astronomy University of Birmingham, UK EAHS2012, Oxford, 2012 March 15.
Seismology of the Sun and solar-like stars Jørgen Christensen-Dalsgaard Institut for Fysik og Astronomi, Aarhus Universitet.
Thanks to Henrietta Swan Leavitt, Harvard CfA November 5th Hommage to Henrietta Leavitt from the CoRoT Team Annie BAGLIN, Merième CHADID,
ASTEROSEISMOLOGY CoRoT session, January 13, 2007 Jadwiga Daszyńska-Daszkiewicz Instytut Astronomiczny, Uniwersytet Wrocławski.
Inversion of rotation profile for solar-like stars Jérémie Lochard IAS 19/11/04.
Catania 09/08SIAMOIS1/26 Benoît Mosser, for the SIAMOIS team Ground-based Doppler asteroseismology after CoRoT and Kepler.
Inside a quaking star: asteroseismic analysis of alpha Centauri Jørgen Christensen-Dalsgaard Institut for Fysik og Astronomi, Aarhus Universitet Teresa.
GONG SoHO 24 A new era of seismology of the Sun and solar-like stars Aix-en-Provence, France Sarbani Basu Yale Unoversity.
Marc Pinsonneault (OSU).  New Era in Astronomy  Seismology  Large Surveys  We can now measure things which have been assumed in stellar modeling 
Nonradial Oscillations. The Science Case:  Stellar Ages - directly for individual stars  Age determination is direct and reliable  Ages to stars which.
PLAnetary Transits and Oscillations of stars Thierry Appourchaux for the PLATO Consortium
C/O abundance in white dwarf interior The asteroseismological data Need higher 12 C+a ? Different convective schemes The effect of 12 C+a So what?
Pulsations and magnetic activity in the IR Rafa Garrido & Pedro J. Amado Instituto de Astrofísica de Andalucía, CSIC. Granada.
July Benoît Mosser Observatoire de Paris LESIA Mixed modes in red giants: a window on stellar evolution Stellar End Products Stellar End Products:
Katrien Uytterhoeven The Kepler space mission: New prospects for δ Sct, γ Dor, and hybrid stars Instituto de Astrofísica de Canarias, Tenerife NMSU, January.
Future of asteroseismology II Jørgen Christensen-Dalsgaard Institut for Fysik og Astronomi, Aarhus Universitet Dansk AsteroSeismologisk Center.
Asteroseismology of the ZZ Ceti star KUV
Scientific aspects of SONG Jørgen Christensen-Dalsgaard Department of Physics and Astronomy Aarhus University.
10/9/ Studying Hybrid gamma Doradus/ delta Scuti Variable Stars with Kepler Joyce A. Guzik (for the Kepler Asteroseismic Science Consortium) Los.
Asteroseismological determination of stellar rotation axes: Feasibility study (COROT AP+CP) L. Gizon(1), G. Vauclair(2), S. Solanki(1), S. Dreizler(3)
June 06, 2013 Putting A Stars into Context: Evolution, Environment, and Related Stars Observational Studies of roAp Stars Mikhail Sachkov Institute of.
Excitation and damping of oscillation modes in red-giant stars Marc-Antoine Dupret, Université de Liège, Belgium Workshop Red giants as probes of the structure.
The asteroseismic analysis of the pulsating sdB Feige 48 revisited V. Van Grootel, S. Charpinet, G. Fontaine P. Brassard, E.M. Green and P. Chayer.
Internal rotation: tools of seismological analysis and prospects for asteroseismology Michael Thompson University of Sheffield
Travis Metcalfe (NCAR) Asteroseismology with the Kepler Mission We are the stars which sing, We sing with our light; We are the birds of fire, We fly over.
Extrasolar Planets and Stellar Oscillations in K Giant Stars Notes can be downloaded from
Stellar Activity in the Kepler Era Tom Ayres (CASA)
A tool to simulate COROT light-curves R. Samadi 1 & F. Baudin 2 1 : LESIA, Observatory of Paris/Meudon 2 : IAS, Orsay.
Modelling high-order g-mode pulsators Nice 27/05/2008 A method for modelling high-order, g-mode pulsators: The case of γ Doradus stars. A. Moya Instituto.
Asteroseismology A brief Introduction
New Surprises from the Microsatellite … aka the Humble space telescope MOST Parameters telescope diameter 15 cm launched 2003 June tracker lost 2006, but…
Precision stellar physics from the ground Andrzej Pigulski University of Wrocław, Poland Special Session #13: High-precision tests of stellar physics from.
Calibration of CoRoT seismological methods using the star  Boo observed by MOST Marian Doru Suran Astronomical Institute of the Romanian Academy
The Empirical Mass Distribution of Hot B Subdwarfs derived by asteroseismology and other means Valerie Van Grootel (1) G. Fontaine (2), P. Brassard (2),
CW9 - Asteroseismology with HARPS 1 Observations with HARPS Benoît Mosser Obs. Paris, LESIA François Bouchy LAM/OHP/IAP
Asteroseismology and the Time Domain Revolution in Astronomy Marc Pinsonneault Ohio State University Collaborators: The APOKASC team Melissa Ness Marie.
Travis Metcalfe Space Science Institute + Stellar Astrophysics Centre Probing Stellar Activity with Kepler.
Oscillation spectra with regular patterns
Asteroseismology with A-STEP The sun from the South Pole Grec, Fossat & Pomerantz, 1980, Nature, 288, 541.
1. Short Introduction 1.1 Overview of helioseismology results and prospects.
The Saga of Procyon Pierre Demarque Yale University “Stars in Motion” A Symposium in honor of Bill van Altena September
July 12, 2004Pulsating PMS stars Pulsating Pre-Main Sequence Stars in Young Open Clusters K. Zwintz Institute of Astronomy, Univ. Vienna, Austria
Sounding the cores of stars by gravity-mode asteroseismology Valerie Van Grootel (Institut d’Astrophysique, University of Liege, Belgium) Main collaborators.
Subdwarf B stars from He white dwarf mergers Haili Hu.
Asteroseismology of Sun-like Stars
Internal dynamics from asteroseismology for two sdB pulsators residing in close binary systems Valérie Van Grootel (Laboratoire d’Astrophysique de Toulouse.
HD and its super-Earth Valerie Van Grootel (University of Liege, Belgium) M. Gillon (U. Liege), D. Valencia (U. Toronto), N. Madhusudhan (U. Cambridge),
Takashi Sekii Division of Solar and Plasma Astrophysics and Hinode Science Center NAOJ Rotation of KIC
Notes: In many of the Fourier transforms the frequency is given in c/d = cycles per day. To convert to  Hz multiply numbers by HD has a period.
Solar-like Oscillations in other Stars or The only way to test directly stellar structure theory I.Scaling Relations II. Results.
Leuven and Nijmegen Universities p. 1 Mode identification from time series of high-resolution high signal-to-noise spectroscopy 1. Aerts et al. (1992),
Asteroseismology of Kepler
Asteroseismic Modeling Portal (AMP) Development
Asteroseismology of solar-type stars
Theoretical Interpretation of Power Spectra of Stellar Oscillations
ASTEROSEISMOLOGY OF LATE STAGES OF STELLAR EVOLUTION
Solar-like oscillations with HARPS …and SOPHIE
Search and Characterization
Presentation transcript:

The Real Music of the Spheres Asteroseismology The Real Music of the Spheres

Sir Arthur Stanley Eddington: The Internal Constitution of the Stars 1926 At first sight it would seem that the deep interior of the sun and stars is less accessible to scientific investigation than any other region of the universe. Sir Arthur Eddington (1882 – 1944)

Our telescopes may probe farther and farther into the depths of space; but how can we ever obtain certain knowledge of that which is hidden behind substantial barriers?

What appliance can pierce through the outer layers of a star and test the conditions within?

Asteroseismology

3D oscillations – stars radial modes Cepheids P1/P0= 0.7 string P1/P0= 0.33

Cepheid variables Cepheid Horn by Zoltan Kollath & Geza Kovács, Konkoly Observatory, Budapest; Robert Buchler, Florida

A giant solar-like oscillator http://www.lcse.umn.edu/

Asteroseismology

Angular structure of the modes n = number of radial nodes  = total number of surface nodes m = number of surface nodes that are lines of longitude  – m = number of surface nodes that are lines of latitude

Dipole modes l=1, m=-1 l=1, m=0 l=1, m=+1

Quadrupole modes l=2, m=-2 l=2, m=-1 l=2, m=0

Rotation of the sun

p modes and g modes J. P. Cox, 1980, Theory of Stellar Pulsation, Princeton University Press.

p modes and g modes p modes g mode (n,) = (8,100), (8,2) Gough et al., 1996, Science, 272, 1281

The sun as a star - BiSON

The sun as a star - GOLF large separation small separation

An asteroseismic HR diagram

Solar-like Oscillations in  Centauri Bedding, T., et al. 2004, ApJ, 614, 380 UVES & UCLES 42 oscillation frequencies ℓ = 1-3 Mode lifetimes only 1-2 days Noise level = 2 cm s-1!

Modelling  Cen A and B Stellar model in good agreement with the astrometric, photometric, spectroscopic and asteroseismic data t = 6.52 ± 0.30 Gyr Initial Y = 0.275 ± 0.010 Initial Z/X = 0.043 ± 0.002 Radii of both stars determined with high precision (errors smaller than 0.3%) compatible with interferometric results of Kervella et al. (differences smaller than 1%) Eggenberger, P., Charbonnel, C., Talon, S., Meynet, G., Maeder, A., Carrier, F., Bourban, G. 2004, A&A, 417, 235

Oscillations and planets Stellar activity, convection and pulsation are “noise” to planet-hunters Planets are “noise” to asteroseismologists The two fields are not just complementary It is mandatory to do both together at cm s-1 precision

 Arae V = 5.15 G3IV-V Prot = 22 days 14 M planet; Porb = 9.55 days 43 p-modes detected 8-day single-site HARPS study Bouchy, F., Bazot, M., Santos, N. C., Vauclair, S., Sosnowska, D., 2005, A&A, 440, 609

 Ara b : giant Msini = 1.67 Jupiter masses a = 1.5 AU Porb = 654.5 days e = 0.31  Ara c : giant Msini = 3.1 Jupiter masses a = 4.17 AU Porb = 2986 days e = 0.57  Ara d : ?? Msini = 14 Earth masses a = 0.09 AU Porb = 9.55 days e = 0

 Arae – the 14 M planet Bouchy, F., Bazot, M., Santos, N. C., Vauclair, S., Sosnowska, D., 2005, A&A, 440, 609

 Arae – ~8-min pulsations Bouchy, F., Bazot, M., Santos, N. C., Vauclair, S., Sosnowska, D., 2005, A&A, 440, 609

 Arae Bouchy, F., Bazot, M., Santos, N. C., Vauclair, S., Sosnowska, D., 2005, A&A, 440, 609

Resolving pulsations in the atmospheres of roAp stars Don Kurtz Vladimir Elkin Gautier Mathys

Theoretical expectation  = 0.7  = 0.1 Saio, 2005, MNRAS, 360, 1022

HD 101065 BaII NdIII

 ~ 10-5  ~ 10-2

HD99563

 ~ 10-5  ~ 10-2  << 10-5

Gautschy, Saio & Harzenmoser, 1998, MNRAS, 301, 31

HD154708 Hubrig, S., Nesvacil, N., Schöller, M., North, P., Mathys, G., Kurtz, D. W., Wolff, B., Szeifert, T., Cunha, M. S., Elkin, V. G., 2005, A&A, 440, L37

HD154708 Kurtz, D. W., Elkin, V. G., Elkin, V. G., Mathys, G., Hubrig,  Wolff, B., Savanov, I., 2006, MNRAS, submitted

We are seeing the roAp star atmospheres in more detail than is possible for any star other than the sun

White dwarfs – g-mode pulsators

PG 1159-035

PG 1159-035 Tsurf = 123,000 - 124,000 K; log g  7 1000  f  2600 Hz; 385  P  1000 s 125 frequencies; >100 modes M = 0.586 ± 0.003 M the star is compositionally stratified

BPM 37093 DAV M = 1.09 M Teff = 11730 K Partially crystallized C-O core Metcalfe, T. S., Montgomery, M. H., Kanaan, A. 2004, ApJ, 605, 133 Kanaan et al., 2005, A&A, 432, 219 Brassard & Fontaine, 2005, ApJ, 622, 572

BPM 37093

p modes: EC 14026 stars - sdBV

PG 1336 + 018

p modes:  Cephei stars

HD 129929 = V836 Cen 20-yr multicolour photometry Core overshooting with aOV = 0.1 Non-rigid rotation: 4 times faster near core Aerts et al., 2003, Science, 300, 926 Asteroseismology of HD129929: Core overshooting and nonrigid rotation

g modes: SPB stars

Continuous coverage - MOST HD163830 SPB star V = 9.3 B5II/III 37 days coverage 20 frequencies detected

HD 163830 Aerts, C.; De Cat, P.; Kuschnig, R.; Matthews, J. M.; Guenther, D. B.; Moffat, A. F. J.; Rucinski, S. M.; Sasselov, D.; Walker, G. A. H.; Weiss, W. W., 2006, ApJ, 642, L65

HD 163830 Aerts, C.; De Cat, P.; Kuschnig, R.; Matthews, J. M.; Guenther, D. B.; Moffat, A. F. J.; Rucinski, S. M.; Sasselov, D.; Walker, G. A. H.; Weiss, W. W., 2006, ApJ, 642, L65

Dome C - Concordia

Seeing 2003-2004: statistics 0.10 Seeing min 0.54 Median seeing 5.22 50% 0.5 0.1 0.3 0.5 1 3 Seeing distribution (log-normal) 0.10 Seeing min 0.54 Median seeing 5.22 Seeing max 0.65 Mean seeing (arcsec) 0.39 Std deviation 17148 N data

What appliance can pierce through the outer layers of a star and test the conditions within? Asteroseismology

Stellarmusicno1 Stellar acoustics as input for music composition Zoltán Kolláth Konkoly Observatory, Budapest, Hungary Jenő Keuler Institute for Musicology, Budapest, Hungary http://www.konkoly.hu/staff/kollath/stellarmusic/

Photometry - HR 1217 WET Xcov20 = 14 mag precision Kurtz et al., 2005, MNRAS, 358, 651

What can you do with the frequencies in roAp stars? – HR 1217

A model and prediction Cunha, M. 1999, PhD thesis, Cambridge Cunha, M. Gough, D., 2001, MNRAS, 319, 1020 Bigot et al. 2000, A&A, 356, 218

HR 1217 photometric campaigns

HR 1217 photometric campaigns