AAS #233 Dissertation Talk - Planetary Archaeology: Exploring the Planet Population of Evolved Stars

Transcript

1. Planetary Archaeology: Exploring Planets Transiting Evolved Stars Samuel Grunblatt, Daniel Huber, Eric Gaidos, Eric Lopez Institute for Astronomy, University of Hawaii—Manoa, Honolulu, HI skg3@hawaii.edu www.ifa.hawaii.edu/~skg @skgrunblatt
2. Distribution of Kepler target stars: mostly Sunlike Kepler Huber+ (2014) @skgrunblatt skg3@hawaii.edu
3. K2: Extension to the NASA Kepler Mission high precision photometry from space (~30-100 ppm precision) 80 day observing campaigns, 30 minute cadence community chosen targets @skgrunblatt
4. Distribution of K2 target stars: more M stars, more giants Huber+ (2016) @skgrunblatt skg3@hawaii.edu
5. Why should you care about planets orbiting giant stars? @skgrunblatt skg3@hawaii.edu
6. To solve long-standing planet inflation mysteries Can planets be inflated at late times? (Burrows+2000, Bodenheimer+2001, Lopez+2016, Grunblatt+ 2016, Grunblatt+2017) @skgrunblatt skg3@hawaii.edu Why should you care about planets orbiting giant stars?
7. To solve long-standing planet inflation mysteries Can planets be inflated at late times? (Burrows+2000, Bodenheimer+2001, Lopez+2016, Grunblatt+ 2016, Grunblatt+2017) To study planet evolution: as star evolves, planets must react inspiral, circularization, engulfment timescales still unknown (Villaver+2014, Fuller 2017, MacLeod+ 2018, Grunblatt+ 2018) @skgrunblatt skg3@hawaii.edu Why should you care about planets orbiting giant stars?
8. To solve long-standing planet inflation mysteries Can planets be inflated at late times? (Burrows+2000, Bodenheimer+2001, Lopez+2016, Grunblatt+ 2016, Grunblatt+2017) To study planet evolution: as star evolves, planets must react inspiral, circularization, engulfment timescales still unknown (Villaver+2014, Fuller 2017, MacLeod+ 2018, Grunblatt+ 2018) To understand stellar variability: key to getting better star/planet parameters & finding currently undetectable planets with future missions motivates new models to characterize stellar variability (Grunblatt+2015, Grunblatt+2017, Jones+2018) @skgrunblatt skg3@hawaii.edu Why should you care about planets orbiting giant stars?
9. A Search for Giants Orbiting Giants with K2 ➤ >10,000 Low Luminosity Red Giant Branch (LLRGB) targets ➤ Transit detection limit: ~9 Rsun ➤ K2 limit for asteroseismology: 283 μHz (~3 Rsun) ➤ Temperature limits: 4500—5500 K 
 (avoids horizontal branch stars) Huber+ (2016) @skgrunblatt skg3@hawaii.edu
10. Asteroseismic stellar parameters: Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
11. Asteroseismic stellar parameters: 2542 LLRGB stars in K2 LLRGB stars Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
12. Seeing Double with K2: Two Remarkably Similar Planets Orbiting Red Giant Branch Stars Grunblatt+ (2017)
13. Grunblatt+ (2017) Seeing Double with K2:… @skgrunblatt skg3@hawaii.edu
14. Seeing Double with K2:… Rs = 3.85 +/- 0.13 R⊙ Ms = 1.08 +/- 0.08 M⊙ Rs = 4.20 +/- 0.14 R⊙ Ms = 1.16 +/- 0.12 M⊙ Grunblatt+ (2017) @skgrunblatt skg3@hawaii.edu
15. ] ] uncorrelated + correlated noise Seeing Double with K2:… @skgrunblatt Grunblatt+ (2017) @skgrunblatt skg3@hawaii.edu
16. Combined transit + GP models Grunblatt+ (2017) Simple Harmonic Oscillator GP Squared Exponential GP Used squared exponential and simple harmonic oscillator GP kernel functions to account for granulation & oscillation noise @skgrunblatt skg3@hawaii.edu
17. Grunblatt+ (2017) Seeing Double with K2:… Rs = 3.85 +/- 0.13 R⊙ Ms = 1.08 +/- 0.08 M⊙ Rp = 1.30 +/- 0.07 RJ Rs = 4.20 +/- 0.14 R⊙ Ms = 1.16 +/- 0.12 M⊙ Rp = 1.31 +/- 0.11 RJ @skgrunblatt skg3@hawaii.edu
18. Are my K2 planets inflated? Yes. Lopez & Fortney (2016) @skgrunblatt skg3@hawaii.edu
19. Data implies significant post-MS planet heating. But how? delayed cooling ] re-inflation Are they re-inflated? Probably. Grunblatt+ (2017) @skgrunblatt skg3@hawaii.edu
20. delayed cooling re-inflation Are they re-inflated? Probably. Grunblatt+ (2017) ] @skgrunblatt skg3@hawaii.edu Data implies significant post-MS planet heating. But how?
21. delayed cooling ] re-inflation Are they re-inflated? Probably. Kepler-422b: 1.15 Msun 0.43 MJ 7.89 days Grunblatt+ (2017) @skgrunblatt skg3@hawaii.edu Data implies significant post-MS planet heating. But how?
22. delayed cooling ] re-inflation Grunblatt+ (2017) Are they re-inflated? Probably. Kepler-422b: 1.15 Msun 0.43 MJ 7.89 days @skgrunblatt skg3@hawaii.edu Data implies significant post-MS planet heating. But how?
23. Why should you care about planets orbiting giant stars? To solve long-standing planet inflation mysteries Can planets be inflated at late times? (Burrows+2000, Bodenheimer+2001, Lopez+2016, Grunblatt+ 2016, Grunblatt+2017) @skgrunblatt skg3@hawaii.edu
24. Why should you care about planets orbiting giant stars? To solve long-standing planet inflation mysteries Can planets be inflated at late times? (Burrows+2000, Bodenheimer+2001, Lopez+2016, Grunblatt+ 2016, Grunblatt+2017) To study planet evolution: as star evolves, planets must react inspiral, circularization, engulfment timescales still unknown (Villaver+2014, Fuller 2017, MacLeod+ 2018, Grunblatt+ 2018) @skgrunblatt skg3@hawaii.edu
25. Grunblatt et al. (2017) Seeing Double with K2: what can RVs tell us? Mp = 0.48 +/- 0.07 MJ Mp = 0.49 +/- 0.06 MJ @skgrunblatt skg3@hawaii.edu
26. They’re eccentric! (e~0.3) @skgrunblatt Grunblatt+ (2018) skg3@hawaii.edu
27. They’re eccentric! (e~0.3) Grunblatt+ (2018) @skgrunblatt skg3@hawaii.edu
28. Do Close-In Planets Orbiting Evolved Stars Prefer Eccentric Orbits? Grunblatt+ (2018)
29. Do close-in giant planets orbiting evolved stars prefer eccentric orbits? Grunblatt+ (2018) @skgrunblatt
30. Do close-in giant planets orbiting evolved stars prefer eccentric orbits? e = 0.15 +0.08-0.04 Grunblatt+ (2018) @skgrunblatt
31. Do close-in giant planets orbiting evolved stars prefer eccentric orbits? e = 0.06 +0.02-0.01 e = 0.15 +0.08-0.04 Grunblatt+ (2018) @skgrunblatt
32. Do close-in giant planets orbiting evolved stars prefer eccentric orbits? Grunblatt+ (2018) ? @skgrunblatt
33. Giant Planet Occurrence Within 0.2 AU of Low Luminosity Red Giant Branch Stars Grunblatt+ (in prep.)
34. Asteroseismic stellar parameters: 2542 LLRGB stars in K2 LLRGB stars Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
35. LLRGB Injection/Recovery Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
36. LLRGB Survey Completeness Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
37. LLRGB Planet Occurrence Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
38. LLRGB Planet Occurrence Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
39. LLRGB Planet Occurrence Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
40. LLRGB Planet Occurrence planet occurrence decreases with radius around MS stars… Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
41. LLRGB Planet Occurrence …but seems to increase with radius around evolved stars! planet occurrence decreases with radius around MS stars… Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
42. What’s next?
43. Better statistics with TESS! Grunblatt (2018) @skgrunblatt skg3@hawaii.edu
44. >10x as many LLRGB planets (Campante+ 2016, Barclay+ 2018) Grunblatt (2018) @skgrunblatt skg3@hawaii.edu
45. Test re-inflation dependencies on star, planet properties @skgrunblatt Campante+ (2016), Barclay+ (2018), Grunblatt (2018) skg3@hawaii.edu
46. Test migration dependencies on star, planet properties @skgrunblatt skg3@hawaii.edu Campante+ (2016), Barclay+ (2018), Grunblatt (2018)
47. Foreman-Mackey+ (2017) Kepler TESS Better statistics with TESS: 100x as many targets! ~103 targets ~105 targets: 100x increase! skg3@hawaii.edu @skgrunblatt skg3@hawaii.edu
48. Foreman-Mackey+ (2017) Kepler TESS Better statistics with TESS: 100x as many targets! ~103 targets ~105 targets: 100x increase! real TESS data from eleanor (Feinstein+ in prep.)! @skgrunblatt skg3@hawaii.edu
49. Better statistics with TESS: more RV followup possible @skgrunblatt skg3@hawaii.edu
50. Better statistics with TESS: more RV followup possible @skgrunblatt skg3@hawaii.edu
51. Better statistics with TESS: more RV followup possible @skgrunblatt skg3@hawaii.edu planets or oscillations? need more data!
52. Summary: you should care about planets orbiting giant stars. To solve planet inflation mysteries Can planets be inflated at late times? (Burrows+2000, Bodenheimer+2001, Lopez+2016, Grunblatt+ 2016, Grunblatt+2017) To study planet migration: as star evolves, planets must react inspiral, circularization, engulfment timescales still unknown (Villaver+2014, Fuller 2017, MacLeod+ 2018, Grunblatt+ 2018) To understand stellar variability: key to measuring better star/planet parameters and finding currently undetectable planets with future missions motivates new models to characterize stellar variability (Grunblatt+2015, Grunblatt+2017, Jones+2018) skg3@hawaii.edu @skgrunblatt ifa.hawaii.edu/~skg
53. Thanks!
55. Extra Slides
56. LLRGB Injection/Recovery Grunblatt+ (in prep.)
57. LLRGB Injection/Recovery (<6 R☉ ) Grunblatt+ (in prep.)
58. K2 Survey Completeness Grunblatt+ (in prep.)
59. K2 Survey Completeness (<6 R☉ ) Grunblatt+ (in prep.)
60. LLRGB Planet Occurrence Grunblatt+ (in prep.)
61. LLRGB Planet Occurrence (<6 R☉ ) Grunblatt+ (in prep.)
62. LLRGB Planet Occurrence Grunblatt+ (in prep.) planet occurrence decreases with radius around MS stars… …but seems to increase with radius around evolved stars!
63. LLRGB Planet Occurrence planet occurrence decreases with radius around MS stars… …but seems to increase with radius around evolved stars! Grunblatt+ (in prep.)
64. Appendix. Why are K2-97b, K2-132b so similar? 0.01 0.10 1.00 10.00 planet mass (Jupiters) 0.0 0.2 0.4 0.6 0.8 1.0 survey bias factor Short answer: probably survey bias * intrinsic planet occurrence
65. Appendix. Why is planet transit depth poorly constrained? Different lightcurves treat systematics differently. Somewhat accounted for with GP model Grunblatt+ (2016)
66. Asteroseismic stellar parameters: are they accurate? Calibrated asteroseismic relations with interferometry (~5% agreement), eclipsing binaries (5-10% agreements). Soon, calculating bolometric fluxes and radii from spectra, and Gaia parallaxes. ~350 bolometric fluxes in hand now. Grunblatt+ (in prep.)