Pulsations and planets at late stages of stellar evolution
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1 at late stages of stellar evolution 1,2 1 Eberhard-Karls-Universität Tübingen 2 Georg-August-Universität Göttingen Kepler Kolloquium, November Subdwarf B stars 3 PG 1159 white dwarfs
2 at late stages of stellar evolution 1,2 1 Eberhard-Karls-Universität Tübingen 2 Georg-August-Universität Göttingen Kepler Kolloquium, November Subdwarf B stars 3 PG 1159 white dwarfs
3 Collaborators Georg-August-Universität Göttingen Dreizler, Lutz, Stahn (now MPS), Kruspe, Beeck (now MPS), Traulsen, Loeptien, Glatzel, Huber Eberhard-Karls-Universität Tübingen Nagel, Werner PG 1159 white dwarfs Friedrich-Alexander-Universität Erlangen-Nürnberg Heber, Falter, Tillich subluminous B stars INAF Istituto Nazionale di AstroFisica, Neapel/Turin Silvotti subluminous B stars University of Arizona, Tucson Steward Observatory Green observations of sdbs Université de Montréal Fontaine, Charpinet (at Toulouse), Randall (now ESO) pulsation theory of sdbs
4 Stellar models Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars self-gravitating fluid sphere described by stellar structure equations conservation of mass conservation of momentum conservation of energy transport of energy as well as properties of stellar matter equation of state energy production opacity
5 Probing stellar interiors Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars : infer inner structure of stars from oscillatory eigenmodes non-radial modes particularly useful two limiting cases of gravo-acoustic modes:
6 Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars the equilibrium solution temperature, pressure, density and chemical composition as a function of a spatial radial coordinate
7 Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars Deviations from the equilibrium solution temperature, pressure, density and chemical composition as a function of a spatial radial coordinate Lamb frequency p modes Brunt-Väisälä frequency g modes
8 Helio- and asteroseismology Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars comparison of full frequency spectrum ν nlm to theoretical predictions (forward modelling) requires high frequency resolution, many modes, mode identification parameters for the models: stellar mass, T eff or L, chemical composition and stratification, rotation, magnetic field need appropriate theory for convection, equation of state, opacities allows to probe interior physics
9 Helio- and asteroseismology Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars
10 Helio- and asteroseismology Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars
11 Science with pulsating stars Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars useful to study... depth of the convection zone in solar-like stars Classical pulsators: driving, opacities, rotation, magnetic fields... non-standard feeder channels for white dwarfs overshoot efficiency parameter in PG 1159 white dwarfs (GW Vir, born-again evolutionary scenario) clues about the evolutionary history of subdwarf B stars (sdb), diffusion secular evolution from Ṗ measurements
12 Solar-like pulsators Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars ground-based observations Aerts, Christensen-Dalsgaard, Cunha & KurtzPulsations 2008, SoPh and planets 251, 3
13 Science with pulsating stars Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars useful to study... depth of the convection zone in solar-like stars Classical pulsators: driving, opacities, rotation, magnetic fields... non-standard feeder channels for white dwarfs overshoot efficiency parameter in PG 1159 white dwarfs (GW Vir, born-again evolutionary scenario) clues about the evolutionary history of subdwarf B stars (sdb), diffusion secular evolution from Ṗ measurements
14 Science with pulsating stars Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars useful to study... depth of the convection zone in solar-like stars Classical pulsators: driving, opacities, rotation, magnetic fields... non-standard feeder channels for white dwarfs overshoot efficiency parameter in PG 1159 white dwarfs (GW Vir, born-again evolutionary scenario) clues about the evolutionary history of subdwarf B stars (sdb), diffusion secular evolution from Ṗ measurements
15 Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars
16 Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars Herwig 2005, ARAA 43, 435
17 Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars Dorman et al. 1993, ApJ 419, 596
18 Stars as gravo-acoustic resonant cavities Forward modelling Evolved stars Green, Fontaine, Hyde et al. 2008, ASPC 392, Østensen 2009, CoAst 159, 75
19
20 short-period sdb variable stars short pulsations, periods of a few minutes driving: κ mechanism due to Z bump opacity accumulated by diffusion = coherent pulsations Kilkenny et al. 1997, MNRAS 285, 640 Charpinet et al. 1996, ApJL, 471, 103 Dreizler, Schuh, Deetjen et al. 2002, A&A 386, 24
21 short-period sdb variable stars short pulsations, periods of a few minutes driving: κ mechanism due to Z bump opacity accumulated by diffusion = coherent pulsations Randall, Fontaine, Brassard & Charpinet 2008, JPhCS 118, 2022 Han et al. 2003, MNRAS 341, 669
22 PG1716 stars (lpsdbvs) slower pulsations, periods of min same κ mechanism, lower amplitudes 30 objects known g mode pulsators Kilkenny et al. 1997, MNRAS 285, 640 Green, Fontaine, Reed,..., Schuh,... et al. 2003, ApJ Letters 583, 31
23 PG1716 stars (lpsdbvs) slower pulsations, periods of min same κ mechanism, lower amplitudes 30 objects known g mode pulsators Kilkenny et al. 1997, MNRAS 285, 640 Green, Fontaine, Reed,..., Schuh,... et al. 2003, ApJ Letters 583, 31
24 Kilkenny et al. 1997, MNRAS 285, 640 Green, Fontaine, Reed,..., Schuh,... et al. 2003, ApJ Letters 583, 31
25 Dreizler, Schuh, Deetjen et al. 2002, A&A 386, 2 49 Schuh, Huber, Dreizler et al. 2006, A&AL 4 45, 31
26 hybrid pulsators with p- and g-modes simultaneously great potential for asteroseismology Schuh, Huber, Dreizler et al. 2006, A&AL 4 45, 31 Lutz, Schuh, Silvotti et al. 2009, A&A 496, 469
27 hybrid pulsators with p- and g-modes simultaneously great potential for asteroseismology Schuh, Huber, Dreizler et al. 2006, A&AL 4 45, 31 Lutz, Schuh, Silvotti et al. 2009, A&A 496, 469
28 Mode identification degree l complex spectrum of frequencies ν strong constraint for models (forward modelling)
29 Mode identification degree l additional constraint from degree l complex spectrum of frequencies ν strong constraint for models (forward modelling)
30 l, ν diagram for stars pulsation frequency ν photometry degree l of pulsation mode geometric consideration for mode identification complementary spectroscopic methods brightness cosθ velocity cos 2 θ cosθ area cosθ area cosθ projected velocity light-to-velocity ratio differs for different degrees l
31 l, ν diagram for stars light-to-velocity ratio differs for different degrees l wavelength dependency of amplitude differs for different degrees l BUSCA
32 l, ν diagram for stars light-to-velocity ratio differs for different degrees l
33 l, ν diagram for stars light-to-velocity ratio differs for different degrees l = simultaneous measurement of light (brightness change) and velocity (radial velocity change) for PG Falter, Heber, Dreizler, Schuh et al. 2003, A&A 401, 289 O Toole, Heber, Jeffery,..., Schuh,... et al. 2005, A&A 440,667 Stahn 2005, Diplomarbeit, Georg-August-Universität Göttingen Tillich, Heber, O Toole,..., Schuh,... et al. 2007, A&A 473, 219
34 Time series of optical spectra deviations from mean spectral line profile Tillich, Heber, O Toole,..., Schuh,... et al. 2007, A&A 473, 219
35 Time series of optical spectra phase relations deviations from mean spectral line profile phase relations radial velocity versus temperature variation: π/3 check: radial velocity versus log g variation: π/2 points to non-adiabatic pulsational behaviour further result: strongest pulsation corresponds to l=1 instead of l=0 Tillich, Heber, O Toole,..., Schuh,... et al. 2007, A&A 473, 219
36 Pulsational radial velocity variation upper limits for line profile variations in V391 Pegasi Kruspe 2009, Diplomarbeit, Georg-August-Universität Göttingen
37 Pulsational radial velocity variation upper limits for line profile variations in V391 Pegasi will need E-ELT Kruspe 2009, Diplomarbeit, Georg-August-Universität Göttingen subdwarf B stars are hot, but compact and hence faint objects
38 Timing method - Ṗ as constraint for models
39 Timing method - Ṗ as constraint for models
40 Timing method - Ṗ as constraint for models
41 O C diagrams example: pulsations as regular clock
42 O C diagrams example: pulsations as regular clock
43 O C diagrams example: pulsations as regular clock clock slows down or accelerates due to secular evolution
44 O C diagrams example: pulsations as regular clock clock slows down or accelerates due to secular evolution
45 O C diagrams example: pulsations as regular clock clock slows down or accelerates due to secular evolution
46 O C diagrams example: pulsations as regular clock clock slows down or accelerates due to secular evolution previously measured secular Ṗ for pulsating sdbs:
47 O C diagram for V391 Pegasi f 1 = µHz Silvotti, Janulis, Schuh et al. 2002, A&A 389, 180 Silvotti, Schuh, Janulis et al. 2007, Nature 449, 189
48 O C diagram for V391 Pegasi f 1 = µHz Silvotti, Janulis, Schuh et al. 2002, A&A 389, 180 Silvotti, Schuh, Janulis et al. 2007, Nature 449, 189
49 O C diagram for V391 Pegasi f 1 = µHz Silvotti, Janulis, Schuh et al. 2002, A&A 389, 180 Silvotti, Schuh, Janulis et al. 2007, Nature 449, 189
50 O C diagram for V391 Pegasi f 1 = µHz f 2 = µhz Silvotti, Janulis, Schuh et al. 2002, A&A 389, 180 Silvotti, Schuh, Janulis et al. 2007, Nature 449, 189
51 Coherent pulsations as timing signal Data points compared to mean model
52 Exoplanets: radial velocity versus timing
53 Exoplanets: radial velocity versus timing
54 Exoplanets: radial velocity versus timing time delay of ±5.3 s ˆ= projected semi-major axis of 5.3 light seconds
55 Exoplanets: radial velocity versus timing time delay of ±5.3 s ˆ= projected semi-major axis of 5.3 light seconds
56 Exoplanets: radial velocity/ pulsation timing time delay of ±5.3 s ˆ= projected semi-major axis of 5.3 light seconds
57 Pulsar planets
58 Pulsar planets Wolszczan A. & Frail D., 1992, Nature, 355, 145
59 Exoplanet search with the timing method
60 Exoplanet search with the timing method goal Find more planets like V 391 Pegasi b method of pulsations in subdwarf B stars advantage Timing method can fill gap: sensitive to planets in wide orbits applicable to evolved stars follow-up Characterisation of target stars monitored mode splitting chromatic amplitudes time-dependent spectroscopy
61 Exoplanet search with the timing method goal Find more planets like V 391 Pegasi b method of pulsations in subdwarf B stars advantage Timing method can fill gap: sensitive to planets in wide orbits applicable to evolved stars follow-up Characterisation of target stars monitored mode splitting chromatic amplitudes time-dependent spectroscopy
62 EXOTIME preliminary results Timing method - long-term stability of the pulsations in HS Loeptien 2009, Bachelorarbeit, Georg-August-Universität Göttingen
63 EXOTIME preliminary results Timing method - long-term stability of the pulsations in HS Loeptien 2009, Bachelorarbeit, Georg-August-Universität Göttingen HS : Lutz, PhD thesis, on-going
64 Exoplanets: radial velocity / eclipse timing time delay of ±5.3 s ˆ= projected semi-major axis of 5.3 light seconds
65 Timing of binary eclipses Lee et al. 2009, AJ 137, 3181 discovery of two planetary-mass objects around HW Vir
66 Timing of binary eclipses Qian et al. 2009, ApJ Letters 695, 163 discovery of a brown dwarf around HS Drechsel, Heber, Napiwotzki,..., Schuh,... et al. 2001, A&A 379, 893
67 Timing of binary eclipses Kruspe, Schuh & Traulsen 2007, IBVS 5796, 1 Qian et al. 2009, ApJ Letters 695, 163 discovery of a brown dwarf around HS Drechsel, Heber, Napiwotzki,..., Schuh,... et al. 2001, A&A 379, 893
68 Beyond extrasolar planet science fate of planetary systems: first or second generation planets? pulsation timing (V 391 Peg) eclipse timing (HW Vir, HS ) radial velocity planet around the subdwarf B star HD : Geier, Edelmann, Heber & Morales-Rueda 2009, ApJL, 702, 96 origin of subdwarf B stars binarity decisive influence of low-mass companions on RGB evolution complementary to insights from asteroseimology and Ṗ KEPLER/KASC program; target list small due to limited field Silvotti, Handler, Schuh et al. 2009, CoAst 159, 97 ground-based observations remain important morphology of blue horizontal branch
69 Renaissance of an old idea suggested second parameter influencing the (blue) horizontal branch morphology in globular clusters and elliptical galaxies Age of the globular cluster Deep helium mixing and radiative levitation Large He abundance or fast rotation Stellar density in the cluster Planets enhancing mass loss on the Red Giant Branch Soker 1998, AJ 116, 1308
70 Renaissance of an old idea suggested second parameter influencing the (blue) horizontal branch morphology in globular clusters and elliptical galaxies Age of the globular cluster Deep helium mixing and radiative levitation Large He abundance or fast rotation Stellar density in the cluster Planets enhancing mass loss on the Red Giant Branch Soker 1998, AJ 116, 1308
71 Born-again scenario Dynamic mass determination Mass-radius relation Hot hydrogen-deficient white dwarfs GW Vir pulsators
72 Born-again scenario Dynamic mass determination Mass-radius relation
73 Born-again scenario Dynamic mass determination Mass-radius relation
74 Born-again scenario Dynamic mass determination Mass-radius relation
75 Born-again scenario Dynamic mass determination Mass-radius relation Mass determinations with different methods frequencies ν pulsation models T eff, log g (stellar atmosphere modelling) evolutionary models asteroseismic and spectroscopic masses differ by up to 10%
76 Born-again scenario Dynamic mass determination Mass-radius relation SDSS2125: a PG 1159 close binary system consistency check with simple physics, no complicated assumptions
77 Born-again scenario Dynamic mass determination Mass-radius relation SDSS2125: a PG 1159 close binary system hot white dwarf and late-type main sequence companion reflection effect periodic brightness variation Nagel, Schuh, Kusterer et al. 2006, A&A Letters 448, 25 Schuh, Traulsen, Nagel et al. 2008, AN 329, 376
78 Born-again scenario Dynamic mass determination Mass-radius relation SDSS2125: a PG 1159 close binary system hot white dwarf and late-type main sequence companion reflection effect periodic brightness variation Nagel, Schuh, Kusterer et al. 2006, A&A Letters 448, 25 Schuh, Traulsen, Nagel et al. 2008, AN 329, 376
79 Born-again scenario Dynamic mass determination Mass-radius relation SDSS2125: a PG 1159 close binary system radial velocity curves; inclination a priori unknown Beeck 2009, Diplomarbeit, Georg-August-Universität Göttingen inclination from light curve modelling
80 Born-again scenario Dynamic mass determination Mass-radius relation Results I: hot hydrogen-deficient white dwarfs (PG 1159) DONE Frequency spectra of GW Vir pulsators, asteroseismic mass determination TODO alternative mass determination ESO: VLT
81 Born-again scenario Dynamic mass determination Mass-radius relation Results I: hot hydrogen-deficient white dwarfs (PG 1159) DONE Frequency spectra of GW Vir pulsators, asteroseismic mass determination TODO alternative mass determination in the only definite PG 1159 close binary system ESO: VLT
82 Born-again scenario Dynamic mass determination Mass-radius relation Results I: hot hydrogen-deficient white dwarfs (PG 1159) DONE Frequency spectra of GW Vir pulsators, asteroseismic mass determination TODO alternative mass determination in the only definite PG 1159 close binary system independent check of the results through measurement of the predicted gravitational redshift in the white dwarfs potential well ESO: VLT
83 Results II: subdwarf B stars RESULTS OUTLOOK SUMMARY (sdb) Search for rapidly pulsating subdwarf B stars discovery of g modes in subdwarf B stars discovery of hybrid pulsators (p+g modes) in subdwarf B stars from long-term monitoring of the pulsations in V391 Pegasi: slow changes in the two main frequencies due to expansion of the star: P 1 =(1.46±0.07) P 2 =(2.05±0.26) discovery of a massive gas giant planet (M sin i=3.2m Jupiter ) in a 1.7 AU orbit, orbit period 3.2a planet survived the red giant phase of its host star measured frequency spectra, frequency changes, and discovery of stellar, sub-stellar and planetary sdb companions:
84 Results II: subdwarf B stars RESULTS OUTLOOK SUMMARY (sdb) Search for rapidly pulsating subdwarf B stars discovery of g modes in subdwarf B stars discovery of hybrid pulsators (p+g modes) in subdwarf B stars Sun: observation of g modes not confirmed yet white dwarfs: observation of p modes not successful yet from long-term monitoring of the pulsations in V391 Pegasi: slow changes in the two main frequencies due to expansion of the star: P 1 =(1.46±0.07) P 2 =(2.05±0.26) discovery of a massive gas giant planet (M sin i=3.2m Jupiter ) in a 1.7 AU orbit, orbit period 3.2a planet survived the red giant phase of its host star measured frequency spectra, frequency changes, and discovery of stellar, sub-stellar and planetary sdb companions:
85 Results II: subdwarf B stars RESULTS OUTLOOK SUMMARY (sdb) Search for rapidly pulsating subdwarf B stars discovery of g modes in subdwarf B stars discovery of hybrid pulsators (p+g modes) in subdwarf B stars Sun: observation of g modes not confirmed yet white dwarfs: observation of p modes not successful yet from long-term monitoring of the pulsations in V391 Pegasi: slow changes in the two main frequencies due to expansion of the star: P 1 =(1.46±0.07) P 2 =(2.05±0.26) direct observation of stellar evolution discovery of a massive gas giant planet (M sin i=3.2m Jupiter ) in a 1.7 AU orbit, orbit period 3.2a planet survived the red giant phase of its host star measured frequency spectra, frequency changes, and discovery of stellar, sub-stellar and planetary sdb companions:
86 Results II: subdwarf B stars RESULTS OUTLOOK SUMMARY (sdb) Search for rapidly pulsating subdwarf B stars discovery of g modes in subdwarf B stars discovery of hybrid pulsators (p+g modes) in subdwarf B stars Sun: observation of g modes not confirmed yet white dwarfs: observation of p modes not successful yet from long-term monitoring of the pulsations in V391 Pegasi: slow changes in the two main frequencies due to expansion of the star: P 1 =(1.46±0.07) P 2 =(2.05±0.26) direct observation of stellar evolution discovery of a massive gas giant planet (M sin i=3.2m Jupiter ) in a 1.7 AU orbit, orbit period 3.2a planet survived the red giant phase of its host star measured frequency spectra, frequency changes, and discovery of stellar, sub-stellar and planetary sdb companions: empirical constraints for theoretical evolutionary scenarios
87 Results II: subdwarf B stars RESULTS OUTLOOK SUMMARY (sdb) Search for rapidly pulsating subdwarf B stars discovery of g modes in subdwarf B stars discovery of hybrid pulsators (p+g modes) in subdwarf B stars Sun: observation of g modes not confirmed yet white dwarfs: observation of p modes not successful yet from long-term monitoring of the pulsations slow changes in the two main frequencies due to expansion of the star: P 1 =(1.46±0.07) P 2 =(2.05±0.26) direct observation of stellar evolution discovery of a massive gas giant planet (M sin i=3.2m Jupiter ) in a 1.7 AU orbit, orbit period 3.2a planet survived the red giant phase of its host star measured frequency spectra, frequency changes, and discovery of stellar, sub-stellar and planetary sdb companions: empirical constraints for theoretical evolutionary scenarios
88 KEPLER mission: RESULTS OUTLOOK SUMMARY useful tool to do asteroseismology; KEPLER/KASC programs main objective is exoplanet search with transit method young stars and main sequence bias
89 RESULTS OUTLOOK SUMMARY KEPLER mission: transits, transits, transits...!
90 RESULTS OUTLOOK SUMMARY KEPLER mission: transits, transits, transits...! Kepler s Optical Phase Curve of the Exoplanet HAT-P-7b Borucki, Koch, Jenkins et al. 2009, Science 325, 709
91 RESULTS OUTLOOK SUMMARY Convergence of instrumentation
92 RESULTS OUTLOOK SUMMARY Convergence of instrumentation
93 RESULTS OUTLOOK SUMMARY Investigation of stellar and planetary systems -exoplanet-connection for solar-like pulsators accurate radii for (solar-like) host stars of transiting exoplanets -exoplanet-connection for post-rgb stars fate of planetary systems known planets around extreme horizontal branch stars: first or second generation? origin of subdwarf B stars second parameter for HB in GC Characterisation of post-agb stars
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