Towards Space Solar Power - Examining Atmospheric Interactions of Power Beams with the HAARP Facility

In the most common space solar power (SSP) system architectures, solar energy harvested by large satellites in geostationary orbit is transmitted to Earth via microwave radiation. Currently, only limited information about the interactions of microwave beams with energy densities of several tens to hundreds of W/m$^2$ with the different layers of the atmosphere is available. Governmental bodies will likely require detailed investigations of safety and atmospheric effects of microwave power beams before issuing launch licenses for SSP satellite systems. This paper proposes to collect representative and comprehensive data of the interaction of power beams with the atmosphere by extending the infrastructure of the High Frequency Active Auroral Research Program (HAARP) facility in Alaska, USA. Estimates of the transmission infrastructure performance as well as measurement devices and scientific capabilities of possible upgrade scenarios will be discussed. The proposed upgrade of the HAARP facility is expected to deliver a wealth of data and information which could serve as a decision base for governmental launch licensing of SSP satellites, and which can be used in addition to deepen public acceptance of SSP as a large-scale renewable energy source. Copyright 2014 IEEE. Personal use of this material is permitted. Permission from IEEE must be obtained for all other uses, in any current or future media, including reprinting/republishing this material for advertising or promotional purposes, creating new collective works, for resale or redistribution to servers or lists, or reuse of any copyrighted component of this work in other works.Comment: 7 pages, 3 figures; to be published in IEEE Xplore, in Proceedings to IEEE Aerospace 2014 Conference, Mar 1 - 8, 2014, Big Sky, MT, US

Implementing TOPbase/Iron Project: Continuous Absorption from Fe II

We discuss implementation of TOPbase and Iron Project opacities for stellar spectral codes. We use a technique employed by Peach, where a Boltzmann-averaged cross section is calculated for selected temperatures, and the opacity obtained from double interpolation in temperature and wavelength. It is straightforward to include {\it all} levels for which cross sections have been calculated. Boltzmann-averaged cross sections for Fe II show a local maximum between 1700 and 2000[A]. We suggest this feature arises from 3d^5 4snl to 3d^5 4pnl transitions within Fe II. IUE spectra of iron-rich CP stars show local minima in this region. Theoretical calculations of a representative stellar continuum demonstrate that Fe II photoionization contributes significantly to the observed minima.Comment: 6 pages, 5 figures. See http://www.astro.lsa.umich.edu/users/cowley/paper2r for better definition figure

Two-Pulse Ionization Injection into Quasi-Linear Laser Wakefields

We describe a scheme for controlling electron injection into the quasi-linear wakefield driven by a guided drive pulse via ionization of a dopant species by a collinear injection laser pulse with a short Rayleigh range. The scheme is analyzed by particle in cell simulations which show controlled injection and acceleration of electrons to an energy of 370 MeV, a relative energy spread of 2%, and a normalized transverse emittance of 3.0 {\mu}m. This is an arXiv version of the original APS paper. It should be cited as N. Bourgeois, J. Cowley, and S. M. Hooker, Phys. Rev. Lett. 111, 155004 (2013). APS link here: http://link.aps.org/doi/10.1103/PhysRevLett.111.155004Comment: 5 pages, 4 figure

Dynamical detection of three triple stellar systems in open clusters

We present a kinematic analysis of three triple stellar systems belonging to two open clusters: CPD-60{\deg}961 and HD66137 in NGC2516, and HD315031 in NGC6530. All three systems are hierarchical triples with a close binary bound to a third body in a wider orbit, whose presence is detected through velocity variations of the close binary barycentre. Orbital parameters are derived from radial velocity curves. Absolute parameters for all stars are estimated assuming cluster membership. Some dynamical and evolutionary aspects of these systems are discussed, particularly the possible influence of Kozai cycles. The two systems of NGC2516 have similar orbital configurations with inner periods of 11.23 d and 8.70 d and outer periods of 9.79 yr and 9.24 yr. We report also radial velocity measurements of the components of the visual binary CPD-60{\deg}944 in NGC2516. Including results from previous works, this cluster would harbor 5 hierarchical triples. The young system HD315031 has an inner binary with a period of 1.37 d and a very eccentric (e=0.85) outer orbit with a period of 483 d. Possible dynamical evolutionary scenarios are discussed. Long-term radial velocity monitoring is highlighted as strategy for the detection of subsystems with intermediate separations, which are hard to cover with normal spectroscopic studies or visual techniques.Comment: 9 pages, 5 figures. Accepted by Monthly Notices of the Royal Astronomical Societ

Modem design for a MOBILESAT terminal

The implementation is described of a programmable digital signal processor based system, designed for use as a test bed in the development of a digital modem, codec, and channel simulator. Code was written to configure the system as a 5600 bps or 6600 bps QPSK modem. The test bed is currently being used in an experiment to evaluate the performance of digital speech over shadowed channels in the Australian mobile satellite (MOBILESAT) project

Polytechnic Instructors as Scholars: Developing a Culture that Embraces Scholarly Activity

This Organizational Improvement Plan (OIP) proposes a leadership solution to develop a culture that embraces faculty scholarly activity at a large Canadian polytechnic institution. The recent advent of two baccalaureate degrees at this diploma-offering institute brought with it the provincial government stipulation that faculty teaching in degree programs must be continually engaged in scholarly activity. A previous unsuccessful implementation of this requirement addressed the functional, managerial aspects of conducting research, however faculty were unprepared for the cultural shift necessary to transform them from polytechnic instructors to scholarly polytechnic instructors. Though the requirement to research remains, early attempts at support have been abandoned, leaving degree faculty and their academic chairs adrift. By creating a centralized institutional research hub and involving stakeholders in the process, material and informational supports would then help shift the scholarly culture towards acceptance and compliance. This OIP underscores the importance of following a prescribed change leadership process that considers both the strategic and cultural aspects of change (Bolman & Deal, 2013; Harris, 1996; Kezar, 2014; Martin, 1992: Prosci, 2016). It couches these ideas and proposals in consideration of the existing, predominant governance structure at the institute, one of transformational, distributed, and ethical leadership (Gaubatz & Ensminger, 2015; House, 1971; Kidder, 1995; Kotter, 2007; Northouse, 2016). This OIP may be adapted to similar contexts at similar institutions, as well as to other change leadership problems where the tendency has been to focus on strategy rather than strategy + cultural change. Keywords: scholarly activity, research, culture, faculty, instructors, polytechnic, problem of practice, transformational leadership, distributed leadershi

Search of X-ray emission from roAp stars: The case of gamma Equulei

The detection of X-ray emission from Ap stars can be an indicator for the presence of magnetic activity and dynamo action, provided different origins for the emission, such as wind shocks and close late-type companions, can be excluded. Here we report on results for gamma Equu, the only roAp star for which an X-ray detection is reported in ROSAT catalogs. We use high resolution imaging in X-rays with Chandra and in the near-infrared with NACO/VLT that allow us to spatially resolve companions down to ~1" and ~0.06" separations, respectively. The bulk of the X-ray emission is associated with a companion of gamma Equu identified in our NACO image. Assuming coevality with the primary roAp star (~900 Myr), the available photometry for the companion points at a K-type star with ~0.6 M_sun. Its X-ray properties are in agreement with the predictions for its age and mass. An excess of photons with respect to the expected background and contribution from the nearby companion is observed near the optical position of gamma Equu. We estimate an X-ray luminosity of log L_x [erg/s] = 26.6 and log(L_x/L_bol) = -7.9 for this emission. A small offset between the optical and the X-ray image leaves some doubt on its association with the roAp star. The faint X-ray emission that we tentatively ascribe to the roAp star is difficult to explain as a solar-like stellar corona due to its very low L_x/L_bol level and the very long rotation period of gamma Equu. It could be produced in magnetically confined wind shocks implying a mass loss rate of ~10^(-14) M_sun/yr or from an additional unknown late-type companion at separation ~0.4". If confirmed by future deeper X-ray observations this emission could point at the origin for the presence of radioactive elements on some roAp stars.Comment: Accepted for publication in Astronomy & Astrophysics (5 pages

The effect of small streamwise velocity distortion on the boundary layer flow over a thin flat plate with application to boundary layer stability theory

Researchers show how an initially linear spanwise disturbance in the free stream velocity field is amplified by leading edge bluntness effects and ultimately leads to a small amplitude but linear spanwise motion far downstream from the edge. This spanwise motion is imposed on the boundary layer flow and ultimately causes an order-one change in its profile shape. The modified profiles are highly unstable and can support Tollmein-Schlichting wave growth well upstream of the theoretical lower branch of the neutral stability curve for a Blasius boundary layer