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IAC science with the prototype SONG node at Tenerife Katrien Uytterhoeven

IAC science with the prototype SONG node at Tenerife Katrien Uytterhoeven. research group ‘ Solar and Stellar Seismology and Extrasolar planet searches’. (7 staff, 2 PostDocs, 3 PhD). Interests in SONG: * the Sun-as-a-star * solar-like stars * red giants * SdB stars * δ Sct, γ Dor

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IAC science with the prototype SONG node at Tenerife Katrien Uytterhoeven

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  1. IAC science with the prototype SONG node at Tenerife Katrien Uytterhoeven

  2. research group ‘Solar and Stellar Seismology and Extrasolar planet searches’ (7 staff, 2 PostDocs, 3 PhD) Interests in SONG: * the Sun-as-a-star * solar-like stars * red giants * SdB stars * δ Sct, γ Dor *β Cep, SPB * OB supergiants * binaries with pulsating components * follow-up of planet candidates Seismology planets

  3. Massive main-sequence pulsators Katrien Uytterhoeven = γ Dor, δ Sct, SPB, β Cep Seismic study requires identified (l,m) modes! Problem: mode-ID does not rely on regularity of frequency spectrum δ Sct HD50844

  4. Mode-ID via line-profile analysis! (l,m) * amplitude and phase distribution across line-profile * velocity moments • GOAL:SONG RV time-series • mode-identification! • b) test and improveseismicmodels

  5. Sun-as-a-star: SONG and Mark-I Pere L. Pallé Mark-I * operational at Obs. Teide since 1976 * full-time monitoring since 1984 * RV of the Sun throughpotassium KI 769.9 nm line * sampling rate: 2sec

  6. GOAL: daytime solar spectra with SONG a) compare simultaneous (same site!) Mark-I and SONG observations (resample to same sampling rate) b) evaluate quality and sensitivity of SONG solar observations

  7. Planet transits Brandon Tingley Use SONG photometry to confirm transit candidates through color changes during transit See talk by Brandon!

  8. > 50 staff scientists > 65 post-docs > 35 PhD students Interests in SONG from IAC research groups other than the group on ‘Solar and Stellar Seismology and Extrasolar planet searches’

  9. i. Wavelength variations in Solar spectral lines Carlos Allende Prieto twilight sky spectrum HET McDonald observatory * 1 yr solar orbit ampl=0.507 km s-1 * 1 d Earth orbit (not well covered) + other deviations! ΔT = 1750 days

  10. Origin of deviations? * changes in granulation properties along solar cycle * presence of planets e.g. Jupiter: 13 m s-1 over 12yr GOAL: twilight sky spectra with SONG and I2 cell a) investigate wavelength stability of the solar spectrum b) demonstrate that deviations due to a Jupiter-size planet can unambigously be found c) study stellar activity

  11. ii. Low mass X-ray binaries Rémon Cornelisse * Compact Binaries (Porb~hrs), primary is compact object (neutron star, black hole). * Roche-lobe overflow, matter accreted via accretion disk. * Inner accretion disk gives rise to X-rays. * optical emission due to Reprocessing of X-rays in outer accretion disk * Different optical wavelengths probe different parts of the outer accretion disk

  12. Large night to night changes in lightcurve morphology Goal:~1 week continuous multi-colour photometric monitoring with the SONG network a) understand the origin of the lightcurve changes b) understand physics of the accretion disk Origin?changes in accretion disk due to precession or the presence of a warp?

  13. iii. Classical Novae at maximum light Alessandro Ederoclite Nova = thermonuclear explosions on surface of white dwarf accreting mass in a close binary * brightening (< V=10mag few weeks) T Pyx, lightcurve * FeII or He/N line absorption * mysterious absorption systems (THEA) Mag questions: * origin of absorption lines? * model that fits at all wavelengths ? MJD - 2450000

  14. T Pyx, FIES spectra 15.04.2011 GOAL: few SONG spectra per day (without I2 cell) during max light of novae follow-up optical thick and thin phase a) describe chemistry b) describe dynamics of explosion Time 30.05.2011

  15. iv. Chemical analysis of EBs Carlos Allende Prieto Well-detached EBs are best calibrators for models of stellar structure and evolution accurate orbital parameters, M*, R* ! BUT! spectral chemical analysis is lacking! • GOAL: • SONG spectra(without I2 cell) of well-known, bright, well-detachedEBsat max separation • derivemetallicity and chemicalabundances of binary components • calibratemodelsstellar structure & evolution

  16. v. Multiple populations in globular clusters Antonino Milone Many globular clusters show multiple sequences! • GOAL: • SONG spectra of bright stars in GCs (filling program) • derive chemical and dynamical properties • and try to solve: • abundance anomalies • multiple sequences • horizontal branch morphology CMD of NGC 2808 with isochrones

  17. vi. macroturbulent broadening in OB supergiants Sergio Simón Díaz OB SGs show extra line broadening: ‘macrotubulence’ origin? pilot study! signature of collective effect of pulsations?!

  18. GOAL: time-series of SONG spectra of bright OB supergiants • understand ‘macroturbulence’ • improve atmosphere models of OB SGs • first seismic studies of OB SGs! promising!

  19. IAC science many interesting filling programs and additional SONG science programs for SONG-OT!

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