A5067199980- Astro and Planetary Science
- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Astronomy and Astrophysical Research
- High-pressure geophysics and materials
- Advanced Graph Theory Research
- Force Microscopy Techniques and Applications
- Geological and Geochemical Analysis
- Crystal Structures and Properties
- Mesoporous Materials and Catalysis
- Vehicle Routing Optimization Methods
- Animal and Plant Science Education
- Silicone and Siloxane Chemistry
- Electronic and Structural Properties of Oxides
- Optimization and Packing Problems
- Complex Network Analysis Techniques
- Advanced Optical Network Technologies
- Astronomical and nuclear sciences
- Atmospheric Ozone and Climate
- Magnetic Properties and Applications
- Geography Education and Pedagogy
- Economic Growth and Productivity
- Advanced X-ray and CT Imaging
- Environmental Education and Sustainability
- Planetary Science and Exploration
The Ohio State University
2019-2024
Abstract The two primary observable quantities of an exoplanet—its mass and radius—alone are not sufficient to probe a rocky exoplanet’s interior composition mineralogy. To overcome this, host-star abundances the planet-building elements (Mg, Si, Fe) typically used as proxy for planet’s bulk composition. majority small exoplanet hosts, however, do have available abundance data. Here we present open-source ExoPlex mass–radius–composition solver. Unlike previous mass–radius solvers, calculates...
Abstract The bulk density of a planet, as measured by mass and radius, is result planet structure composition. Relative proportions iron core, rocky mantle, gaseous envelopes are degenerate for given density. This degeneracy reduced planets without significant when the assumed to be differentiated core in which fraction (CMF) first-order description planet’s A CMF may derived both from assuming reflects host star’s major rock-building elemental abundances (Fe, Mg, Si). Contrasting measures,...
Abstract We investigate and compare the composition of M-dwarf planets in systems with only one known planet (“singles”) to those residing multiplanet (“multis”) fundamental properties their host stars. restrict our analysis directly measured masses radii, which comprise a total 70 planets: 30 singles 40 multis 19 systems. bulk densities for full sample, includes ranging size from 0.52 R ⊕ 12.8 , find that single have significantly lower on average than multis, we cannot attribute selection...
We report quantitative measurements of optically detected ferromagnetic resonance (ODFMR) thin films that use nitrogen-vacancy (NV) centers in diamonds to transduce FMR into a fluorescence intensity variation. To uncover the mechanism responsible for these signals, we study ODFMR as 1) vary separation NV from ferromagnet (FM), 2) record center longitudinal relaxation time $T_1$ during FMR, and 3) material properties FM. Based on results, propose following ODFMR. Decay scattering driven,...
We present a reanalysis of the K2-106 transiting planetary system, with focus on composition K2-106b, an ultra-short period, super-Mercury candidate. globally model existing photometric and radial velocity data derive mass radius for K2-106b $M_{p} = 8.53\pm1.02~M_{\oplus}$ $R_{p} 1.71^{+0.069}_{-0.057}~R_{\oplus}$, which leads to density $\rho_{p} 9.4^{+1.6}_{-1.5}$ $\rm g~cm^{-3}$, significantly lower value than previously reported in literature. use planet interior models that assume...
Abstract Lava worlds are a potential emerging population of Super-Earths that on close-in orbits around their host stars, with likely partially molten mantles. To date, few studies have addressed the impact magma observed properties planet. At ambient conditions, is less dense than solid rock; however, it also more compressible increasing pressure. Therefore, unclear how large-scale oceans affect planet observables, such as bulk density. We update ExoPlex , thermodynamically self-consistent...
Abstract Exoplanets with radii between those of Earth and Neptune have stronger surface gravity than Earth, can retain a sizable hydrogen-dominated atmosphere. In contrast to gas giant planets, we call these planets dwarf planets. The James Webb Space Telescope (JWST) will offer unprecedented insight into Here, investigate the detectability ammonia (NH 3 , potential biosignature) in atmospheres seven temperate using various JWST instruments. We use petitRadTRANS PandExo model planet simulate...
Abstract Using mass–radius composition models, small planets ( R ≲ 2 ⊕ ) are typically classified into three types: iron-rich, nominally Earth-like, and those with solid/liquid water and/or atmosphere. These classes generally expected to be variations within a compositional continuum. Recently, however, Luque & Pallé observed that potentially Earth-like around M dwarfs separated from lower-density population by density gap. Meanwhile, the results of Adibekyan et al. hint iron-rich FGK...
Abstract We present analytic estimates of the fractional uncertainties on mass, radius, surface gravity, and density a transiting planet, using only empirical or semi-empirical measurements. first express these parameters in terms transit photometry radial velocity (RV) observables, as well stellar radius R ⋆ , if required. In agreement with previous results, we find that, assuming circular orbit, gravity planet ( g p ) depends RV parameters, namely period P depth δ semi-amplitude K duration...
The two primary observable quantities of an exoplanet--its mass and radius--alone are not sufficient to probe a rocky exoplanet's interior composition mineralogy. To overcome this, host-star abundances the planet-building elements (Mg, Si, Fe) typically used as proxy for planet's bulk composition. majority small exoplanet hosts, however, do have available abundance data. Here we present open-source ExoPlex mass-radius-composition solver. Unlike previous mass-radius solvers, calculates core...
The bulk density of a planet, as measured by mass and radius, is result planet structure composition. Relative proportions iron core, rocky mantle, gaseous envelopes are degenerate for given density. This degeneracy reduced planets without significant when the assumed to be differentiated core in which fraction (CMF) first-order description planet's A CMF may derived both from assuming reflects host star's major rock-building elemental abundances (Fe, Mg, Si). Contrasting measures,...
Online modes of teaching and learning have gained increased attention following the COVID-19 pandemic, resulting in education delivery trends likely to continue for foreseeable future. It is therefore critical understand implications student outcomes their interest or affinity towards subject, particularly water science classes, where educators traditionally employed hands-on outdoor activities that are difficult replicate online. In this study, we share our experiences adapting a...
We investigate and compare the composition of M-dwarf planets in systems with only one known planet (``singles") to those residing multi-planet (``multis") fundamental properties their host stars. restrict our analysis directly measured masses radii, which comprise a total 70 planets: 30 singles 40 multis 19 systems. bulk densities for full sample, includes ranging size from $0.52 R_{\oplus}$ $12.8R_\oplus$, find that single have significantly lower on average than multis, we cannot...
Lava worlds are a potential emerging population of Super-Earths that on close-in orbits around their host stars with likely partially molten mantles. To date, few studies address the impact magma observed properties planet. At ambient conditions is less dense than solid rock; however, it also more compressible increasing pressure. Therefore, unclear how large-scale oceans affect planet observables, such as bulk density. We update ExoPlex, thermodynamically self-consistent interior software,...
We present a reanalysis of the K2-106 transiting planetary system, with focus on composition K2-106b, an ultra-short period, super-Mercury candidate. globally model existing photometric and radial velocity data derive mass radius for K2-106b $M_{p} = 8.53\pm1.02~M_{\oplus}$ $R_{p} 1.71^{+0.069}_{-0.057}~R_{\oplus}$, which leads to density $ρ_{p} 9.4^{+1.6}_{-1.5}$ $\rm g~cm^{-3}$, significantly lower value than previously reported in literature. use planet interior models that assume...