A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation

My talk at Towards Other Earths III, in Porto Portugal, on Monday July 17, at 5:10 PM.
The talk is about our recently submitted paper here:
https://arxiv.org/abs/2307.08959

Note that the HAT-P-67 stellar and planet properties reported on slides 20 and 21 reflect the previously published values from Zhou et al. 2017. Our new paper (link above) slightly refines these values from revised Gaia DR3 distance, use of new isochrones, and more numerous RV samples with HPF (albeit still consistent with an RV non-detection). See the paper for more information.

Slide 38 shows an animation from Thorngren, Lee, & Lopez 2023 available on the HTML version of the ApJ website:
https://iopscience.iop.org/article/10.3847/2041-8213/acbd35

The top-down orbit on slides 28 - 31 is merely a cartoon to emphasize the leading nature ot the tail, and not its actual orbital location-- a genuine planetary wind consistent with the outflow will initially reside at orbital separations closer into the star, and not directly on top of the planet orbit.

Transcript

1. Michael Gully-Santiago The University of Texas at Austin Towards Other Earths III July 17, 2023 Porto, Portugal A Large and Variable Leading Tail of Helium in a Hot Saturn Undergoing Runaway Inflation Caroline V. Morley, Jessica Luna, Morgan MacLeod, Antonija Oklopčić, Aishwarya Ganesh, Quang H. Tran, Zhoujian Zhang, Brendan P. Bowler, William D. Cochran, Daniel M. Krolikowski, Suvrath Mahadevan, Joe P. Ninan, Guðmundur Stefánsson, Andrew Vanderburg, Joseph A. Zalesky, Gregory R. Zeimann Gully-Santiago et al. submitted; on tonight’s arXiv posting
2. The Mass-Radius diagram
3. Why so few inflated sub- Saturns? The Inflated Sub-Saturn Cliff
4. Scenario 1: Nature does not make them. Scenario 2: Nature makes them, but they are unstable. Why so few inflated sub- Saturns?
5. Scenario 1: Migration prevents sub-Saturns from reaching high Teq . Scenario 2: They reach high Teq , but quickly undergo Runaway Inflation. Thorngren & Fortney 2018
6. Scenario 1: Migration prevents sub-Saturns from reaching high Teq . Scenario 2: They reach high Teq , but quickly undergo Runaway Inflation. Thorngren & Fortney 2018 Key question: How efficiently does insolation couple into the interior?
7. Anomalous heating efficiency, ε Thorngren & Fortney 2018 Observationally disfavored Favored Observationally disfavored Agnostic to the physical mechanism causing the anomalous heating Peaks at ~3% for Teq ~ 1600 K Governs the extent of radius inflation
8. The steady state Radius-Mass slope steepens with increasing Teq . Thorngren & Fortney 2018
9. Thorngren & Fortney 2018 The steady state Radius-Mass slope steepens with increasing Teq .
10. Thorngren & Fortney 2018 The steady state Radius-Mass slope steepens with increasing Teq .
11. Thorngren & Fortney 2018 A positive feedback loop ensues.
12. Thorngren & Fortney 2018 A positive feedback loop ensues.
13. Thorngren & Fortney 2018 A positive feedback loop ensues. Losing mass makes you larger, which makes you lose mass faster.
14. Inflated sub-Saturns should exhibit profound mass loss rates. Thorngren & Fortney 2018
15. Inflated sub-Saturns are rare. Thorngren & Fortney 2018
16. This talk: Helium 10833 Å observations of HAT-P-67 b & HAT-P-32 b
17. Habitable Zone Planet Finder (HPF) Helium Exospheres Survey λ = 8100 – 12,800 Å R = 55,000 Hobby Eberly Telescope (HET), Texas, USA HET has fixed-altitude design: not fully-steerable - Restricts available visit times - Restricts available visit durations to <1 hour We get abundant orbital phase coverage: Large orbital phase coverage Visits In–Transit Out-of-Transit HAT-P-32 b 3 18 HAT-P-67 b 7 35
18. Large tails of Helium excess were previously missed due to limited out-of-transit phase coverage. (i.e. self-subtraction of genuine planetary signal) Zhang, Morley, Gully-Santiago et al. 2023 DOI: (10.1126/sciadv.adf8736) Giant tidal tails of helium escaping the hot Jupiter HAT-P-32 b We detect a 12-hour Helium transit. (the white-light transit lasts for 3.1 hours) The sky-projected length of the tails is 53 Rp
19. Large tails of Helium excess arise naturally from Keplerian orbital shear: dayside mass loss precedes the planet nightside mass loss trails the planet Giant tidal tails of helium escaping the hot Jupiter HAT-P-32 b Zhang, Morley, Gully-Santiago et al. 2023 DOI: (10.1126/sciadv.adf8736) 3D MHD simulations estimate Mass Loss at ̇ 𝑴 ~ 1 ×1012 g/s ~ 5 M ⨁ / Gyr
20. HAT-P-67 an F subgiant Zhou et al. 2017
21. HAT-P-67 b a very low density, inflated hot Saturn Zhou et al. 2017
22. HAT-P-67 b with HPF 39 nights over 3 years 13.8 hours of on-sky integration time 152 individual exposures
23. HAT-P-67 b shows conspicuous variability in He I 10833 Å.
24. Up to 10% transit depths.
25. HAT-P-67 b also has an extended ingress.
32. Leading tail resides in the stellar rest frame.
33. Weak trailing tail blueshifts indicating acceleration away from the planet.
34. The leading tail is direct evidence for preferential dayside mass loss.
35. ̇ 𝑴 ~ 2 ×1013 g/s (105 M ⨁ / Gyr ) with 1D Parker Winds models † (p-winds) †Significant uncertainty: - XUV radiation - T0 - 3D effects (streams) - self-shielding Dos Santos et al. 2022 with Mp < 100 M ⨁ implies inflationary timescale 𝜏infl < 1 Gyr
36. What physical mechanisms cause runaway inflation?
37. Ohmic Dissipation and XUV irradiation both predict runaway inflation for hot Saturns Batygin, Stevenson & Bodenheimer 2011 Thorngren, Lee & Lopez 2023
38. Thorngren, Lee & Lopez 2023 XUV irradiation removes hot Saturns from the mass-radius plane. Mass loss is a positive feedback loop near the 0.1 g/cm3 threshold.
39. Ohmic Dissipation and XUV irradiation make different quantitative predictions for inflation timescales. HAT-P-67 b Theory: 𝜏infl ~ 5-50 Myr Observed: 𝜏infl < 1000 Myr
40. XUV irradiation better matches the population of hot Saturns 0.1 g cm-3 threshold divides observed planet sample from sub-Saturn cliff.
41. Conclusions We have detected up to 10% transit depth of He I 10833 Å from HPF spectra of HAT-P-67 b. The excess absorption preceeds the transit by up to 130 planetary radii in a large leading tail. The prominence of this leading tail is direct evidence for preferential dayside mass loss. We estimate a mass loss rate of 2 x 1013 g/s, and lifetime less than a Gyr. This pattern broadly agrees with theoretical predictions and explains the lack of inflated sub-Saturns.
42. blasé interpretable machine learning for high-resolution stellar spectra Gully-Santiago & Morley 2022 github.com/gully/blase - Forward models an entire high-bandwidth échelle spectrum - Treats properties of all 10,000 spectral lines free parameters - Transfer learns from precomputed synthetic spectra à Evaluable semi-empirical templates, extensible to EPRV & activity mitigation
43. blasé interpretable machine learning for high-resolution stellar spectra Gully-Santiago & Morley 2022 github.com/gully/blase - Forward models an entire high-bandwidth échelle spectrum - Treats properties of all 10,000 spectral lines free parameters - Transfer learns from precomputed synthetic spectra à Evaluable semi-empirical templates, extensible to EPRV & activity mitigation
44. We have detected up to 10% transit depth of He I 10833 Å from HPF spectra of HAT-P-67 b. The excess absorption preceeds the transit by up to 130 planetary radii in a large leading tail. The prominence of this leading tail is direct evidence for preferential dayside mass loss. We estimate a mass loss rate of 2 x 1013 g/s, and lifetime less than a Gyr. This pattern broadly agrees with theoretical predictions and explains the lack of inflated sub-Saturns. Conclusions