Bulletin of the American Physical Society
9th Annual Meeting of the Northwest Section of the APS
Volume 52, Number 6
Thursday–Saturday, May 17–19, 2007; Pocatello, Idaho
Session E4: Astronomy, Cosmology, Gravity |
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Chair: E.J. Zita, Evergreen College Room: PSUB South Fork Room |
Saturday, May 19, 2007 2:00PM - 2:36PM |
E4.00001: LISA: Our infrasonic ear to the universe Invited Speaker: The Laser Interferometer Space Antenna (LISA) is a space mission proposed by NASA and ESA for detecting gravitational-wave signals in the sub-milli-hertz to deci-hertz band. LISA will observe a myriad of sources, from galactic compact binaries in our galaxy to supermassive black hole mergers at cosmological distances. In the process, it will map the distribution of the galactic binary population, perform tests of strong gravity, and provide an independent estimate of the Hubble constant. In addition to discussing how LISA will achieve these goals, I will address the primary challenges facing LISA phenomenology, such as (1) the problem of detecting signals from individual sources while battling the source confusion noise from thousands of galactic binaries and (2) modeling the evolution of extreme mass-ratio binary inspirals. I will conclude by discussing the unique role LISA will play in complementing other observatories of the time in pursuit of some interesting astrophysical discoveries. [Preview Abstract] |
Saturday, May 19, 2007 2:36PM - 3:12PM |
E4.00002: Solar dynamo modeling and prediction Invited Speaker: Global-scale solar dynamo models have evolved significantly over the past half century. The model that can most successfully reproduce many global solar cycle features is the so-called 'flux-transport' dynamos. Along with the differential rotation (Omega-effect) and helical turbulence (alpha-effect), another important ingredient in this class of models is the meridional circulation, which works as a conveyor belt and governs the dynamo cycle period as well as the memory of the Sun's past magnetic fields. After describing the physical processes involved in a flux-transport dynamo, we will show how a predictive tool can be built from it that can be used to predict mean solar cycle features by assimilating magnetic field data from previous cycles. We will present our timing and amplitude predictions for upcoming cycle 24. We will close by discussing the sensitivity of our model in predicting N/S asymmetry in solar cycles. [Preview Abstract] |
Saturday, May 19, 2007 3:12PM - 3:30PM |
E4.00003: Coffee Break
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Saturday, May 19, 2007 3:30PM - 3:42PM |
E4.00004: Pulsar Kicks from Electrons in a Large Magnetic Field Ernest Henley We derive the momentum asymmetry given to a proto-neutron star during a time (10-20 s) that the neutrino sphere is near the surface of the star, using the modified Urca process. The electrons are in Landau levels due to the strong magnetic field, and this leads to an asymmetry in the neutrino momentum and thus to a pulsar kick. Our kicks reach 1000 km/s for a $ T = 8.5 \times 10^{10}K$. [Preview Abstract] |
Saturday, May 19, 2007 3:42PM - 3:54PM |
E4.00005: Laboratory Nuclear Astrophysics, viewing the universe from underground. John E. Ellsworth, Steven E. Jones, Lawrence B. Rees, Clark G. Christensen Our sun emits 380 yottawatt, yet the nuclear reactant energies producing that power are very low ($\sim $1 keV). Replication of such reactions in the laboratory produces rates that are nearly impossible to detect. Unlike the historical efforts to understand stellar processes by extrapolating down from higher energy beam experiments, we report efforts to study reactions using low energy reactants. To do so requires specialized equipment and environments. Research to study muon catalysis[1] began at BYU in 1982 in collaboration with INEL and LANL. This led to the 1986 BYU hypothesis that `metals can catalyze d-d fusion' and a theory for heat production in planets[2]. Experiments followed[3-5]. Since the mid 1990s a body of data for the screening potentials of metals has grown out of accelerator experiments[6-10]. [1]Nature 1986 321:p327. [2]J. Phys. G:12:213-221. [3]Nature 338:737-740. [4]SE Jones, Four Corners Fall Meeting, APS, (2004). [5]CMNS 2005, London:World Scientific, p509{\&}p525. [6]Z. Phys. A351:107. [7]JETP Letters, 68:823. [8]Europhys. Lett. 54:449. [9]Eur. Phys. J, A19:283. [10]J. Phys. Soc. Japan, 73:608. [Preview Abstract] |
Saturday, May 19, 2007 3:54PM - 4:06PM |
E4.00006: Laboratory Detection of Cold Dark Matter as Sidereal Dilaton Scattering Data George Soli An experiment designed to prove that the one-way group-velocity of slow-photons does not exist, produces a surprising positive result. The one-way velocity is larger than simple Newtonian velocity addition of the photon's velocity and Earth's velocity relative to the CMB, indicating that the photons must be interacting with something at rest relative to the CMB. That something turns out to be CDM that is the dilaton or Goldstone boson of scale-invariance symmetry-breaking, that is at rest relative to the CMB with a mass greater than our photon's vacuum excitation energy of 3.3 $\mu $eV. This non-classical scattering interaction with dilatonic CDM is mediated by the magnetic fine structure constant (137) discovered as a Morse function critical point in the higher dimensional anti de Sitter space used to model the scattering interaction. The vacuum excitation energy saturates the Ford-Roman quantum inequality implying that the Goldstone boson is also negative pressure dark energy, solving the dark matter-energy coincidence problem. This CDM also solves many other cosmological problems. It has already been argued in the literature that Einstein thought of our measured slow-photon magnetic flux tubes first. [Preview Abstract] |
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