Tenured and Tenure-Track Positions

The Department of Physics at The University of Alabama in Huntsville (UAHuntsville) seeks applicants for six tenure-track faculty positions beginning Fall 2008 at the Assistant Professor Level. The research areas of interest are listed below. Unusually well-qualified candidates will be considered for the rank of Associate Professor. Successful candidates will also hold research appointments in the Center for Space Plasma and Aeronomic Research (CSPAR). Candidates should have a Ph.D. in Physics or a closely related area; a strong commitment to teaching, research, and the mentoring of graduate students; and the ability to contribute effectively to the Department’s undergraduate and graduate programs.

1. Heliospheric physics. Candidates should have the following qualifications and experience: (i) Focused transport theory and experience in applying computer models based on the numerical solution of the focused transport equation to both the problem of anomalous cosmic-ray (ACR) acceleration at the heliospheric termination shock and solar energetic particle (SEP) acceleration at coronal mass ejection driven interplanetary shocks. (ii) At interplanetary shocks, numerical modeling of Alfven wave transport in a nonuniform plasma medium, wave generation by particle anisotropies upstream of shocks as described by quasilinear theory, and nonlinear wave-wave interaction using a diffusion formalism is required. Knowledge of kinetic weak turbulence theory of wave cascading will also be useful. (iii) Modeling of the structural modification of the termination shock within a three fluid context (solar wind, multiply reflected ions, and anomalous cosmic rays) using a kinetic-MHD model is required. This experience should include modeling interstellar pickup ion multiple reflection and acceleration by the cross-shock potential (MRI acceleration mechanism) and the associated shock modification. (iv) Development of the theory of cosmic-ray scattering by MHD turbulence especially in the context of determining acceleration rates of ACRs at the termination shock and the transport of cosmic rays in the outer heliosphere. (vi) Active NASA and/or NSF grants that support research in both solar energetic particle acceleration at interplanetary shocks and anomalous cosmic-ray acceleration at the termination shock. Log Number 08/09-514-1

2. Interplanetary and interstellar plasma turbulence. Candidates should have the following qualifications and experience: (i) Development of self-consistent models and undertaken simulations of coupled plasma-neutral ISM turbulence for the case where plasma and neutral gas are coupled mainly through the process of charge exchange. (ii) Exploration of the self consistent evolution of such a partially ionized system, investigating the role of charge exchange and its influence on spectral transfer, spectral anisotropy, and energy spectra in the context of the inner and outer heliosheath regions of the heliosphere. (iii) Development of an understanding of the observed ISM electron density fluctuation spectra based upon fully 3D compressible magnetohydrodynamic and nearly incompressible (NI) models. (iv) Development various 2D and 3D fluid turbulence codes, especially for the investigation of nearly incompressible hydrodynamic and magnetohydrodynamic turbulence, with MPI parallelization on clusters. (v) Experience in the numerical simulation of whistler wave turbulence, driven-dissipative magnetohydrodynamic turbulence, and anisotropic energy cascades in magnetohydrodynamic turbulence. Log Number 08/09-514-2

3. Particle acceleration and transport. Candidates should have the following qualifications and experience: (i) Development of numerical codes for the modeling of particle acceleration and transport at propagating CME-driven or interplanetary shock waves. This includes the integration of a numerical MHD fluid code (such as ZEUS) that follows the shock propagation along with modeled particle acceleration at the shock front. The particle acceleration code should address (a) Alfven wave generation by particle anisotropies upstream at/near a quasi-parallel shock, and (b) a Non-linear Guiding Theory or related model describing particle transport and acceleration at quasi-perpendicular shocks. The successful candidate will be expected to continue the development of a fully 2D particle acceleration code at an oblique shock. (ii) Modeling specific gradual/impulsive solar energetic particle events. This includes comparing model calculations of proton and heavy ion time intensity profiles and spectra with observations obtained from spacecraft such as ACE, Wind and Ulysses, amongst others. (iii) Investigation of particle transport in a turbulent magnetic field, applying quasi linear theory and the underlying Fokker Planck transport equation to these problems. This includes experience in modeling solar energetic particle transport due to pitch angle scattering using Monte-Carlo codes that are coupled self-consistently to particle acceleration models, especially at shock waves. (iv) Active NASA and/or NSF grants that support research in both solar energetic particle acceleration and transport at CME-driven and/or interplanetary shocks as well as solar flares. A Ph.D. or equivalent degree in physics, astrophysics or a related field within the past 9 years and at least 3 years of post-doc experience. Log Number 08/09-514-3

4. Heliospheric modeling. Candidates should have the following qualifications and experience: (i) Heliospheric modeling, including (a) three-dimensional, self-consistent modeling of the heliosphere, including cosmic-ray transport and acceleration in heliospheric plasmas; (b) self-consistent kinetic modeling of anomalous cosmic ray acceleration and transport at a dynamical termination shock; (c) kinetic modeling of particle acceleration at heliospheric shocks using a focused transport approach; and (d) heliopause evolution and stability. (ii) Strong background in numerical simulations and high performance scientific computing, and experience with distributed-memory (Beowulf-class) system. (iii) Active NASA and/or NSF grants that support research in the 3D modeling of cosmic ray transport and acceleration. Log Number 08/09-514-4

5. Heliospheric and computational physics. Candidates should have the following qualifications and experience: (i) Numerical modeling of the interaction of the nonstationary, three-dimensional heliosphere with the local interstellar medium on the basis of magnetohydrodynamic (MHD), multi-fluid (plasma and neutral fluids), and MHD plasma / kinetic neutrals approaches, where both the plasma and neutral H gas are coupled self-consistently. (ii) The physical processes that occur in the partially ionized plasma of the outer heliospheric solar wind (SW) and local interstellar medium (LISM), such as, charge exchange and collisions between charged and neutral particles, pick-up ion processes, the transport of energetic neutral atoms throughout the heliosphere, heliospheric current sheet behavior, and the propagation of SW disturbances, such as, global merged interaction regions, and corotating interaction regions. (iii) Modeling the filtration of interstellar neutral particles at the heliospheric interface. (iv) Contemporary high-resolution numerical methods for solving hyperbolic systems of conservation laws, including the use and application of adaptive mesh refinement techniques to ensure highly resolved boundaries and structures. (v) Considerable experience in performing extensive, large-scale simulations on modern supercomputers, and have a record of capturing time on machines supported by DOE, NASA, NCSA, NSF and/or other agencies nationwide. (vi) Active NASA and/or NSF grants that support investigation of transient phenomena in the outer heliosphere. Log Number 08/09-514-5

6. Heliospheric modeling and magnetic reconnection. Candidates should have the following qualifications and experience: (i) Kinetic modeling of neutral atoms in the heliosphere using sophisticated computational techniques, such as Monte Carlo methods. This includes the ability to successfully couple such a kinetic neutral atom code to the MHD codes used for solving the ionized component of the heliospheric interface. The candidate should be proficient in the use of Message Passing Interface (MPI), to ensure that the resulting codes are efficiently ported to large scale parallel machines. (ii) Magnetic reconnection, with applications to solar flares and coronal heating. This includes experience in the numerical modeling of magnetic reconnection using Hall-MHD. (iii) Demonstrated capability of securing time on high-speed supercomputers in order to resolve the heliospheric neutral and ionized distributions with sufficient accuracy. (iv) Active NASA and/or NSF research grants that support research on neutral atoms in the heliosphere, including the details of collisional processes between heliospheric atoms and ions. Log Number 08/09-514-6

Applicants should send a resume, a statement of teaching philosophy, a research plan, (unofficial) graduate transcripts, and three letters of recommendation to:

James A Miller, Professor and Chair
Department of Physics
The University of Alabama in Huntsville
Huntsville AL 35899

The log number of the specific position applied for should be referenced in all submitted material. Review of complete applications will begin 11 April 2008 and continue until the positions are filled.

UAHuntsville is an Equal Opportunity Employer/Affirmative Action Employer

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