Bulletin of the American Physical Society
APS April Meeting 2015
Volume 60, Number 4
Saturday–Tuesday, April 11–14, 2015; Baltimore, Maryland
Session H2: Dark Matter III |
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Sponsoring Units: DPF DNP Chair: Laura Reina, Florida State University Room: Holiday 1 |
Sunday, April 12, 2015 8:30AM - 8:42AM |
H2.00001: Stability Analysis of DM-Ice17 Zachary Pierpoint DM-Ice17, a 17 kg sodium iodide prototype detector for the proposed DM-Ice experiment, was deployed in the Antarctic Ice at the geographic South Pole in December 2010, and has been in operation since January 2011. I will present a stability analysis of three years of data, with a focus on sources of noise and time-dependent effects that could mimic or obfuscate a dark matter modulation. Due to the small mass of the detector, the analysis does not significantly probe dark matter regions of interest but does provide further evidence that the Antarctic ice provides an ideal location for dark matter annual modulation searches. [Preview Abstract] |
Sunday, April 12, 2015 8:42AM - 8:54AM |
H2.00002: The speculation of the formation process about dark matter Yongquan Han Rotation makes the radiation of the object convergence, the linear speed of the object decides the degree of convergence about object. The characteristics of the convergence object is: radiation intensity in the process of convergence become stronger, but the radiation radius is getting smaller and smaller, and the radiation will eventually converge in the objects inside, that is the dark matter. To validate that advice: 1, make a luminous ball. 2, The experimenter stay far from the light sphere in the empty night observer, until just can not see the ball or can just see extremely fuzzy (due to the distance, the light is weak and sparse). 3, high speed rotate (the rotation instead of rotate around), when the speed reaches a certain value, if we can see the ball become clear, that remains the light rays bend, radiation get smaller, but in the radiation range, the intensity of radiation become stronger. Verify that the material rotation speed reaching the speed of light, it becomes the inflection point of matter and dark matter, ultra light rotation becomes dark matter. Verify that if an object superluminal rotation, it is the dark matter [Preview Abstract] |
Sunday, April 12, 2015 8:54AM - 9:06AM |
H2.00003: Dark matter or point sources? ~Utilizing the 1-pt PDF to understand the origin of the GeV excess seen by the Fermi LAT detector Natalie Harrison, Jennifer Gaskins An excess of gamma rays from the Inner Galaxy in the Fermi LAT data has been identified. ~This emission has been interpreted as a possible signature of the annihilation of dark matter particles, or as originating from a collection of unresolved point sources, such as gamma-ray millisecond pulsars. ~We explore the clustering properties of the diffuse emission arising from a population of gamma-ray point sources and from the annihilation of dark matter particles in the halo of the Galaxy using the 1-pt probability distribution function of counts in pixels (1pt-PDF, the number of pixels with a specified number of counts as a function of counts); this approach is also known as fluctuation analysis or P(D) analysis. We analyze the 1-pt PDF of the GeV excess within a $+$/- 5 degree box around the Galactic Center. ~For both dark matter and point sources we adopt the spatial distribution and spectrum to fit the GeV excess. ~We determine the contributions to the 1-pt PDF from the Galactic diffuse and isotropic diffuse emissions, dark matter, and point sources, and discuss the implications of this analysis for the origin of the GeV excess.~ [Preview Abstract] |
Sunday, April 12, 2015 9:06AM - 9:18AM |
H2.00004: Multiscale renormalization group methods for effective potentials with multiple scalar fields Zhi-Wei Wang, Tom Steele, Gerry McKeon Conformally symmetric scalar extensions of the Standard Model are particular appealing to reveal the underlying mechanism for electroweak symmetry breaking and to provide dark matter candidates. The Gildener \& Weinberg (GW) method is widely used in these models, but is limited to weakly coupled theories. In this talk, multi-scale renormalization group (RG) methods are reviewed and applied to the analysis of the effective potential for radiative symmetry breaking with multiple scalar fields, allowing an extension of the GW method beyond the weak coupling limit. A model containing two interacting real scalar fields is used as an example to illustrate these multi-scale RG methods. Extensions of these multi-scale methods for effective potentials in models containing multiple scalars with $O(M)\times O(N)$ symmetry will also be discussed. [Preview Abstract] |
Sunday, April 12, 2015 9:18AM - 9:30AM |
H2.00005: Optimization of Geometries for Experimental Searches of Chameleon Scalar Fields Vladimir Skavysh, Muhammad Arif, Chandra Shahi, Robert Haun, Mike Snow, Ke Li, Benjamin Heacock, Albert Young The chameleon scalar field theory is a dynamic model of dark energy. This model is unique in that it gives predictions which can be tested in terrestrial experiments. Here, we consider the prediction that the chameleon field exacts a force on objects in vacuum. Due to symmetry of typical objects, this force is usually miniscule. However, the chameleon force on a single surface can be surprisingly large, which is why we investigate whether there exist geometries for which the net chameleon force on an object is large enough to be measured. Moreover, we consider multi-body systems, such as the setup of the high-frequency short-range gravity experiment at Indiana University (arXiv:hep-ph/0303057v2), which consists of three oscillating parallel plates. [Preview Abstract] |
Sunday, April 12, 2015 9:30AM - 9:42AM |
H2.00006: Search for strongly coupled Chameleon scalar field with neutron interferometry K. Li, M. Arif, D. Cory, R. Haun, B. Heacock, M. Huber, J. Nsofini, D.A. Pushin, P. Saggu, D. Sarenac, C. Shahi, V. Skavysh, M. Snow, A. Young The dark energy proposed to explain the observed accelerated expansion of the universe is not understood. A chameleon scalar field proposed as a dark energy candidate can explain the accelerated expansion and evade all current gravity experimental bounds. It features an effective range of the chameleon scalar field that depends on the local mass density. Hence a perfect crystal neutron interferometer, that measures relative phase shift between two paths, is a prefect tool to search for the chameleon field. We are preparing a two-chamber helium gas cell for the neutron interferometer. We can lower the pressure in one cell so low that the chameleon field range expands into the cell and causes a measurable neutron phase shift while keeping the pressure difference constant. We expect to set a new upper limit of the Chameleon field by at least one order of magnitude. [Preview Abstract] |
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