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A combination of observations, experiments, and modeling are needed to understand the role of planetary interiors on habitability and guide the search for extraterrestrial life.
Transition from a weak and erratic geomagnetic field to a more stable one around 560 million years ago, inferred from palaeomagnetic measurements, suggests that the inner core may have solidified around that time, much later than thought.
The paleomagnetic record is central to our understanding of the history of the Earth. The orientation and intensity of magnetic minerals preserved in ancient rocks indicate the geodynamo has been alive since at least the Archean and possibly the Hadean. A paleomagnetic signature of the initial solidification of the inner core, arguably the singular most important event in core history, however, has remained elusive. In pursuit of this signature we investigate the assumption that the field is a geocentric axial dipole (GAD) over long time scales. We study a suite of numerical dynamo simulations from a paleomagnetic perspective to explore how long the field should be time-averaged to obtain stable paleomagnetic pole directions and intensities. We find that running averages over 20 − 40 kyr are needed to obtain stable paleomagnetic poles with α95 < 10°, and over 40 − 120 kyr for α95 < 5°, depending on the variability of the field. We find that models with higher heat flux and more frequent polarity reversals require longer time averages, and that obtaining stable intensities requires longer time averaging than obtaining stable directions. Running averages of local field intensity and inclination produce reliable estimates of the underlying dipole moment when reversal frequency is low. However, when heat flux and reversal frequency are increased we find that local observations tend to underestimate virtual dipole moment (VDM) by up to 50% and overestimate virtual axial dipole moment (VADM) by up to 150%. A latitudinal dependence is found where VDM underestimates the true dipole moment more at low latitudes, while VADM overestimates the true axial dipole moment more at high latitudes. The cause for these observed intensity biases appears to be a contamination of the time averaged field by non-GAD terms, which grows with reversal frequency. We derive a scaling law connecting reversal frequency and site paleolatitude to paleointensity bias (ratio of observed to the true value). Finally we apply this adjustment to the PINT paleointensity record. These biases produce little change to the overall trend of a relatively flat but scattered intensity over the last 3.5 Ga. A more careful intensity adjustment applied during periods when the reversal frequency is known could reveal previously obscured features in the paleointensity record.
Numerical Dynamo Simulations
Numerical Dynamo Simulations
I use open source dynamo codes (Rayleigh and MagIC) to model magnetohydrodynamics of planetary interiors. My primary application is to Earth's core to investigate the long-time scale evolution of geomagnetic field intensity, orientation, and polarity reversal rate. I am also interested in applications to other terrestrial planets, gas giants, and exoplanets.
I use open source dynamo codes (Rayleigh and MagIC) to model magnetohydrodynamics of planetary interiors. My primary application is to Earth's core to investigate the long-time scale evolution of geomagnetic field intensity, orientation, and polarity reversal rate. I am also interested in applications to other terrestrial planets, gas giants, and exoplanets.
See: Driscoll and Wilson 2018; Driscoll 2016; Driscoll 2015, Driscoll & Olson 2011a, 2009a, 2009b
Planetary Interior Structure & Evolution
Planetary Interior Structure & Evolution
I have developed codes (IDL, Python) to model the internal structure and thermal evolution of Earth-like planets for a range of masses and core/mantle fractions. These codes are being developed to allow variable composition and other features.
I have developed codes (IDL, Python) to model the internal structure and thermal evolution of Earth-like planets for a range of masses and core/mantle fractions. These codes are being developed to allow variable composition and other features.
See: Driscoll & Olson 2011b, Driscoll & Bercovici 2013, 2014, Foley & Driscoll 2016
Carnegie Habitability Project
Carnegie Habitability Project
See: CHP website
Coupling Interiors to Orbits
Coupling Interiors to Orbits
I am a collaborator with the Virtual Planet Lab (U. Washington) where we are developing a code called VPLANET to simulate the coupled astrophysical and geophysical evolution of planets and stars. I am the primary developer of the internal structure, thermal evolution, and radiogenic heating modules of the code.
I am a collaborator with the Virtual Planet Lab (U. Washington) where we are developing a code called VPLANET to simulate the coupled astrophysical and geophysical evolution of planets and stars. I am the primary developer of the internal structure, thermal evolution, and radiogenic heating modules of the code.
Exoplanet Magnetic Field Detection
Exoplanet Magnetic Field Detection
I have developed a preliminary model to predict the radio emission from terrestrial exoplanet magnetic fields and am interested in working to interpret exodynamo emissions (once they are detected).
I have developed a preliminary model to predict the radio emission from terrestrial exoplanet magnetic fields and am interested in working to interpret exodynamo emissions (once they are detected).
See: Driscoll & Olson 2011b, Lazio et al 2016
VPLANET
VPLANET
I am a member of the development team for the code VPLANET. I am the primary developer of physics modules for terrestrial planetary interiors.
I am a member of the development team for the code VPLANET. I am the primary developer of physics modules for terrestrial planetary interiors.
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