1. The Little Satellite that Could... Derek Buzasi Univ. of Washington & Eureka Scientific

2. Introduction “X-ray vision” for stars A brief history of WIRE Some Closeups  Altair  Polaris  Alpha Cir  Procyon  Eclipsing Binaries Future Prospects

3. How do we know anything about the internal structure of the Sun?

4. Coherent motions on the solar surface Leighton (1960) uses Doppler effect to observe oscillatory motion on the Sun  Amplitudes are ~hundreds of meters/sec  Periods are ~5 min (~3 mHz)‏

5. 1975: Things start to get interesting…

6. What are these things? They appear to be acoustic waves traveling in a cavity  The Sun is ringing like a bell The study of these waves is called “helioseismology”

7. Each unique way in which the Sun can oscillate is called a “mode”

8. Modes

10. OK – so what good is all this? (Some real physics at last!)‏ Each mode has a frequency which is characteristic of some “average” sound speed along its travel path  “Low degree” modes penetrate deeply  “High degree” modes sample only the surface By using information from all of the modes, we can model the inside of the Sun! Good news! There are more than a million modes Bad news! There are more than a million modes

11. We can even map the internal rotation

12. …and details of internal convection

13. It would be nice to do this for stars, too… Unfortunately, asteroseismology is much more difficult  Less light (and atmospheric interference)‏  Unresolved sources But astronomers are trying!

14. A little about stars… What we’d like to know  mass, age, composition, rotation rate, internal structure, activity, etc. Ways to find out  cluster stars (common origin)  binary stars (interact via gravity)  field stars (help!) Wider applications?  distance scale, nucleosynthesis, etc.

15. Hertzsprung- Russell (HR) Diagram Remember this?

16. Technical Approaches to Asteroseismology Two Basic Approaches 1. Look for tiny Doppler shifts (~10 cm/s, or parts per billion) in spectral lines from the ground, where we have big telescopes. 2. Look for tiny variations (parts per million) in the stellar luminosity from space, where the atmosphere isn’t a problem.

17. Other Uses for ultra-high-precision photometry Rotational Modulation Granulation (surface signature of convection)‏ Eclipses & transits

18. WIRE = Wide-Field Infrared Explorer 1994: Selected by NASA; IR mission designed to study extragalactic star formation for 4 mos 1999: Pegasus launch on 4 Mar 1999 1999: Primary mission failure on 8 Mar 1999 1999: Conversion to asteroseismology mission begins 30 Apr 1999 May 1999 – Sept 2000: Epoch 1 Dec 2003 – 23 Oct 2006: Epoch 2 Launched 4 Mar 1999; failed 8 Mar 1999

19. The Star Tracker Ball Aerospace CT-601 52 mm aperture 512  512 SITe CCD 7.8°  7.8° field (1 arcmin/pixel)‏ 16-bit ADC Gain 15e - /ADU

20. Epoch I Original mission was 30 April 1999 - 30 September 2000 28 asteroseismology targets; 10 additional targets Primary targets only Mission termination due to lack of funding

21. Epoch II Mission restart New flight software included field rotation, making secondary targets usable

22. Selected Accomplishments Altair  What don’t we know about the brightest star in the northern sky? Polaris  New insights into an old favorite Alpha Cir  Interaction of rotation and oscillations Procyon  Granulation in a solar-like star Eclipsing Binaries  Old wine in new bottles

23. Altair Brightest star in the northern sky Part of the “summer triangle” Sometimes used as a flux standard! WIRE observed for 22 days...

24. Each “frame” represents a 2-day window Overall envelope of variability is ~2 ppt

25. Largest peak is at 15.768 d - 1 ; amplitude 0.42 mmag Altair is the brightest δ Scuti star! Frequency units are “cycles/day” – 15.76 c/d corresponds to roughly 1.5 hours.

26. 9 total modes detected; f 1 is easily identified as the fundamental but other IDs are less clear due to the extremely rapid rotation of the star. HR diagram showing selected models. The two evolutionary tracks depicted correspond to 1.70 solar masses and v = 150 km/s (solid line), and 1.75 solar masses and v = 200 km/s (dashed line). The cross indicates observations. Ages in the shaded area range from 500 to 750 Myr

27. Polaris “North Star” Closest and brightest Cepheid  Amplitude has been dropping for decades  No longer detectable as variable from the ground Observed simultaneously using multiple telescopes  WIRE  SMEI  AST

28. Polaris: Data Quality

29. Oscillation timing is changing: stellar evolution in real time!

30. Alpha Circinis Member of class rapidly oscillating peculiar A-type (roAp) stars  First detected in 1970s with ground-based telescopes  Typical periods are a few minutes  Typical amplitudes are a few parts per thousand or less Alpha Cir has one well-known mode, with a frequency of 2442 mHz

31. Combination of ground & space-based observations

32. Asymmetry in light curve

33. Amplitude of primary mode is variable: rotation!

34. Distance Determination via Asteroseismology

35. Procyon‏ F5 IV (V ~ 0, so one of the brightest stars in the sky)‏ Historically considered one of the best possible stellar targets for asteroseismology  Higher mass, more evolved star is expected to have larger oscillation amplitudes based on theory WIRE analysis by Bruntt, Kjeldsen, Buzasi, Bedding  Two time series totalling ~19 days

36. The light curves of Procyon as seen from WIRE in September 1999 (top) and September 2000 (bottom). Data affected by scattered light have been removed and the correlation with FWHM has been removed. In each panel, only every fifth data point is plotted.

37. Comparisons: WIRE x 2, MOST, Solar The plot shows the smoothed power density spectrum for each data set. PDSs permit direct comparison of different time series, since they take into account the different lengths and resolutions of the data sets. The VIRGO data represent the solar PDS as viewed from space. Note that hydrodynamic models predict Procyon to have somewhat greater granulation “noise” than the Sun does. The excess power in the MOST data appears to be due to an as yet not understood noise source.

38. The granulation timescale and granulation PDs are 750 s and 18 ppm 2 / µHz, while the amplitude of the p- modes are 5, 10, 15 ppm. The four panels show the power density spectrum of the WIRE 2000 time series along with different simulations. Each simulation is the mean of five simulations with different seed numbers. The hatched regions show the 1-σ variation for selected simulations. Simulations for two different white noise levels Simulations have timescales of the granulation of 250, 750, and 1250 s. The timescale of the granulation is 750 s but the granulation power densities (PDs) are 10, 18, and 64 ppm 2 / µHz.

39. Best-fit models WIRE spectra are marked by open box symbols The 1-σ variation of the simulations is shown by the hatched region. WIRE 1999 and 2000 results: Procyon

40. Eclipsing Binaries A classic astronomer’s tool  Orbital timing gives stellar masses  Lengths of eclipses give relative stellar radii  Depths of eclipses give relative stellar temperatures  Shapes of eclipse light curves give atmospheric structure

41. Eclipsing Binaries with WIRE

42. Good (ground-based TT Aur)…

43. Better (WIRE,  Eri)

44. Best! (WIRE,  Aur)

45. But wait, there’s more…

46. Where do we go from here? The future of asteroseismology lies in space!

48. END

49. Fourier Transforms Are Your Friends… (Really!)‏

50. Things get worse: here’s a signal-to-noise ratio of 10…

51. And a signal-to-noise ratio of 0.01… Real data look like this!

53. Amazing Appearing Modes!