A5080982390- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Atmospheric Ozone and Climate
- Astro and Planetary Science
- Advanced Chemical Physics Studies
- Cold Atom Physics and Bose-Einstein Condensates
- Gamma-ray bursts and supernovae
- Aluminum Alloy Microstructure Properties
- Molecular Spectroscopy and Structure
- Animal and Plant Science Education
- Italian Fascism and Post-war Society
- Spectroscopy and Laser Applications
- Quantum, superfluid, helium dynamics
- Science Education and Pedagogy
- Science Education and Perceptions
- Semiconductor materials and devices
- Magnetic and transport properties of perovskites and related materials
- Copper Interconnects and Reliability
- Astronomy and Astrophysical Research
- Astronomical Observations and Instrumentation
University of Virginia
2019-2023
McCormick (United States)
2023
Despite the rich observational results on interstellar magnetic fields in star-forming regions, it is still unclear how dynamically significant are at varying physical scales, because direct measurement of field strength observationally difficult. The Davis-Chandrasekhar-Fermi (DCF) method has been most commonly used to estimate from polarization data. It based assumption that gas turbulent motion driving source distortion via linear Alfv\'en waves. In this work, using MHD simulations...
The complete three-dimensional structure of the magnetic field within molecular clouds has eluded determination despite its high value in determining controlling factors star formation process, as it cannot be directly probed observationally. Considering that inclination relative to plane sky is one major sources depolarization thermal emission from dust clouds, we propose here a new method estimate angle cloud-scale based on statistical properties observed polarization fraction. We test...
Abstract With the recent advent of circular polarization capabilities at Atacama Large Millimeter/submillimeter Array (ALMA), Zeeman effect measurements spectral lines are now possible as a means to directly probe line-of-sight magnetic fields in protoplanetary disks (PPDs). We present modeling study that aims guide physical interpretation these anticipated observations. Using fiducial density structure based on typical ringed disk, we simulate line emission for hyperfine components CN J =...
We compare the structure of synthetic dust polarization with molecular line emission from radiative transfer calculations using a 3-dimensional, turbulent collapsing-cloud magnetohydrodynamics simulation. The histogram relative orientations (HRO) technique and projected Rayleigh statistic (PRS) are considered. In our trans-Alfv\'enic (more strongly magnetized) simulation, there is transition to perpendicular alignment at densities above $\sim$$4 \times 10^{3}$ cm$^{-3}$. This recovered in...
We use the POLARIS radiative transfer code to produce simulated circular polarization Zeeman emission maps of CN $J = 1 - 0$ molecular line transition for two types protostellar envelope magnetohydrodynamic simulations. Our first model is a low mass disk system (box length $L 200\text{ au}$), and our second massive protostar ($L 10^4\text{ au}$) with wind enhanced outflow shell. compute velocity-integrated Stokes $I$ $V$, as well implied $V/I$ percentage, each detector pixel location in...
We compare the structure of synthetic dust polarization with molecular line emission from radiative transfer calculations using a 3-dimensional, turbulent collapsing-cloud magnetohydrodynamics simulation. The histogram relative orientations (HRO) technique and projected Rayleigh statistic (PRS) are considered. In our trans-Alfvénic (more strongly magnetized) simulation, there is transition to perpendicular alignment at densities above $\sim$$4 \times 10^{3}$ cm$^{-3}$. This recovered in most...
Underrepresentation in STEM fields starts early, with elementary students already showing differences based on gender and race their interest science, belief ability to do that personal identity aligns being a scientist. Here we discuss an out-of-school time astronomy program focuses enriching science education under-served school systems promote students' excitement about help them see scientists as people just like them. Before, after, throughout the program, survey perceptions of...
ABSTRACT We use the polaris radiative transfer code to produce simulated circular polarization Zeeman emission maps of cyanide (CN) J = 1–0 molecular line transition for two types protostellar envelope magnetohydrodynamic simulations. Our first model is a low-mass disc system (box length L 200 au), and our second massive protostar (L 104 au) with wind CN-enhanced outflow shell. compute velocity-integrated Stokes I V, as well implied V/I percentage, each detector pixel location in maps....
(1977). Yardstick Gives Way to Meterstick. The Clearing House: A Journal of Educational Strategies, Issues and Ideas: Vol. 51, No. 2, pp. 92-92.