Summer 2020

Fridays at 12:00 PM


June 12, 2020

Speaker: Matthew S. Tarling, University of Otago, New Zealand

Title: Episodic tremor and slip in the geologic record: chemical reactions in serpentinite within the source region of deep episodic tremor

Abstract: Seismic and geodetic studies continue to reveal a diverse spectrum of earthquake behaviour along subduction megathrusts worldwide. This includes “slow fault slip”, which refers to a range of transient phenomena that occur over timescales longer than those of standard earthquakes. Slow slip phenomena include temporally and spatially correlated seismic tremor and slow slip events known as episodic tremor and slip (ETS). Deep ETS occurs in the transitional region between the megathrust seismogenic zone and the deeper, stably sliding zone. A number of hypotheses for the origins of ETS have been proposed. However, the geological processes controlling ETS have yet to be elucidated due to the relatively coarse resolution of geophysical datasets and the lack of direct geological observations from ETS source regions. Most hypotheses invoke contemporaneous stable and unstable frictional sliding accompanied by fluctuations in pore-fluid pressures that promote frictional failure in regions where viscous shear would otherwise occur. As geophysicists and seismologists continue to expand our understanding of slow slip and ETS, a better understanding of the chemo-mechanical processes that act in ETS source regions would provide valuable input for physical models of slow slip and megathrust behaviour. An unresolved problem is whether any of the slow earthquake phenomena documented in active subduction zones can leave a trace that can be resolved and studied in the geological record. I will summarise our current understanding of the possible geological signatures of slow slip and ETS in the rock record. Additionally, I will present field and microstructural observations from the plate boundary-scale Livingstone Fault in New Zealand, which can be used to explore how chemical reactions can promote rock hardening and generate in-situ fluid overpressures. These processes may collectively result in hydrofracturing and a transition from distributed creep to localized brittle faulting, phenomenologically analogous to episodic tremor and slip.

matt


June 16, 2020

Speaker: James Head, Brown University

Title: Noachian Mars Climate: 'Warm and Wet' or 'Cold and Icy'?


June 26, 2020

Speaker: Brandon Johnson, Purdue University

Title: Impact basins as probes of planetary interiors


July 3, 2020

Speaker:

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July 10, 2020

Speaker: Miki Nakajima, Rochester

Title: Consequences of Giant Impacts: Lunar Origin and Magma Ocean Formation

Abstract: The Apollo lunar samples reveal that Earth and the Moon have strikingly similar isotopic ratios, suggesting that these bodies may share the same source materials. This leads to the giant impact hypothesis, suggesting the Moon formed from a disk that was generated by an impact between Earth and a Mars-sized object. This disk would have had high temperature (~ 4000 K), and its silicate vapor mass fraction would have been ~20 wt %. More energetic impact models have been proposed and they produce higher temperatures (~ 6000 K) and vapor mass fractions (~80-90 wt%). Some or most of these models can potentially explain the isotopic similarity. However, these energetic models may face a challenge that has not been considered to date. An initially vapor-rich Moon-forming disk may have trouble forming a large Moon because growing lunar seeds can fall onto Earth in a very short timescale due to a strong headwind from the vapor. This issue could be potentially resolved if a large lunar seed form quickly by streaming instability, which is a clump formation process caused by a spontaneous concentration and gravitational collapse of the particles. Here, we investigate whether the streaming instability can operate in the Moon-forming disk based on the numerical code Athena. Our study finds that this instability can operate in the Moon-forming disk, but the seeds may not be large enough to avoid the strong gas drag. The gas drag effect is negligible for the standard model because the vapor-mass fraction of the disk is small. Thus, our study indicates that the standard giant hypothesis remains a strong candidate for the lunar origin. We also discuss its implication for exomoons. Moreover, we will also discuss a scaling law for the shape and size of an impact-induced magma ocean based on more than 100 giant impact simulations using the method called smoothed particle hydrodynamics (SPH).

 miki


July 17, 2020

Speaker: Megan Mansfield, University of Chicago

Title: Ultra-Hot Jupiters: Revealing the Atmospheres of a Novel Class of Exoplanets

megan

Abstract: Hot Jupiters are compelling targets for thermal emission observations because their high signal-to-noise allows precise atmospheric characterization. Theory originally predicted that cooler planets would show absorption features in their secondary eclipse spectra due to having uninverted atmospheres, while warmer planets would have inverted atmospheres causing emission features in their eclipse spectra. I first discuss our group’s early observations of ultra-hot Jupiters, which led to the realization that these hottest exoplanets are a distinct class with unique high-temperature chemistry. I present new models which take into account this new high-temperature chemistry, and show how they can explain the featureless spectra we observe in many ultra-hot Jupiters. However, observed hot Jupiters still show a surprising level of diversity in their eclipse spectra. To further examine this diversity, I perform a population study of all secondary eclipse observations of hot Jupiters with the Hubble Space Telescope (HST). From this population study I propose that the spectra of hot Jupiters can be explained through compositional diversity in their atmospheres. In the coming years we will have the opportunity to study hot Jupiter atmospheres in even more detail using the James Webb Space Telescope (JWST). In particular, JWST will provide the unique capability to perform spectroscopic eclipse mapping, which will allow us to map the atmospheres of hot Jupiters in three dimensions (latitude, longitude, and altitude). I present a new method to analyze eclipse mapping observations which can be used to interpret these complicated data sets without relying on expectations from circulation models. Finally, I discuss ongoing observations of hot Jupiters which I will be leading in the coming year using both HST and ground-based high-resolution observations.


July 24, 2020

Speaker: Sergio Ruiz, University of Chile

Title: Some observations in the near field of Chilean earthquakes: From nucleation to earthquake rupture process.


July 31, 2020

Speaker: Kelsi Singer, SWRI

Title: New insights into the impact process from lunar secondary craters and the ejecta fragments that made them

Abstract: When an impact crater forms on a planetary surface, fractured pieces of the surface material are ejected and can form their own secondary craters outside of the main, or primary, crater. Secondary craters are found in large numbers on the Moon and other bodies, and they provide evidence of the impact process. The size of secondary craters is related to the size of the ejecta fragment, and the distance of the secondary crater from the primary is related to fragment ejection velocity. We mapped secondary craters around primary craters ranging in size from ~0.83–660 km in diameter using Lunar Reconnaissance Orbiter Camera (LROC) Narrow and Wide Angle Camera images. With this dataset this we were able to investigate the impact process through a new empirical lens, and found a scale-dependence that is not currently accounted for in analytical fragmentation theories. We were also able to compare this data to secondary craters on icy satellites to test for any material dependence. I will give an overview of the morphology of secondary craters and our mapping philosphy, the techniques used to investigate trends in the data, and the new results.


August 7, 2020

Speaker: Matt Siegler, PSI

Title: Planetary Heat Flow: InSight on Mars and InSights into the Moon

Bio: Dr. Matthew Siegler is a research scientist at Planetary Science Institute based in Dallas, TX. He specializes in all things thermal, including thermal modeling, infrared and microwave remote sensing, volatile stability, geothermal heat, and laboratory thermal measurements. He is a Co-I on LRO, InSight, OSIRIS-REx, 2 lunar CLPS instruments, and the upcoming Viper lunar rover. He will be talking about the struggles of measuring geothermal heat flow on Mars and how microwave instruments may aid in future missions. He is father to Jack and June and in the process of making them an awesome treehouse

matt


August 14, 2020

Speaker: Kanani Lee, Lawrence Livermore National Laboratory

Title: Planetary diversity: From diamond planets to hot Jupiters

kanani

Abstract: With more than 3000 planets confirmed outside of our own Solar System, the realization that many are very different from those in our own Solar System lends itself easily to the discussion of plausible planetary compositions and its effect on a planet’s thermochemical evolution. In this talk I’ll bring together astronomical observations and mineral physics experiments to constrain possible exoplanetary interiors in an attempt to move from non-unique mass-radius relationships.


August 21, 2020

Speaker: Laura Wallace, University of Texas

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August 28, 2020

Speaker: Sarah Titus, Carleton College

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September 4, 2020

Speaker: Ben Weiss, MIT

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September 11, 2020

Speaker: Ryan C. Hurley, Johns Hopkins University,

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September 18, 2020

Speaker: Randy Williams, University of Wisconsin-Madison

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