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a14e8bcd653eb874d9c00018fadc10d002ea4c5e | subsection | 2 | 20 | Introduction | REF (c-d)) trace out the unstable
manifold \mathcal {W}_{\mathrm {u}} of the chaotic saddle . Aspects of mixing
in open flows such as residence-time distributions, fractal dimensions
of the mixing pattern, or the dynamics of chemical reactions occurring
in the flow have been related to properties of the chaotic
saddle ... | {
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"raw": "C. Jung, T. Tél, and E. Ziemniak, “Application of scattering chaos to particle transport in a hydrodynamical flow,” Chaos 3, 555 (1993).",
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"Emmanuelle Gouillart",
"Olivier Dauchot",
"Jean-Luc Thiffeault",
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] | [
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b7f0bbae8b1011d5bef00a48fcfd70cc19c27e49 | subsection | 3 | 20 | Introduction | Fromthis moment on, a permanent pattern appears to set in: patterns in (c) and(d) resemble each other very closely, but with a weaker intensity atlonger times.] | {
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} | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
"Emmanuelle Gouillart",
"Olivier Dauchot",
"Jean-Luc Thiffeault",
"Stéphane Roux"
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0db95895d11781e1ea5c1b128004b8bc25521a53 | subsection | 4 | 20 | Experimental set-up and methods | We have designed an experimental device to study mixing in open flows
with two main criteria: (i) a stirring flow that promotes chaotic
advection and is simple enough to draw generic conclusions; and (ii) a
device that is realistic enough to be relevant to applications. To
satisfy the latter criterion, we require the d... | {
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} | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
"Emmanuelle Gouillart",
"Olivier Dauchot",
"Jean-Luc Thiffeault",
"Stéphane Roux"
] | [
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e6018fe97f77d8363017644147500a9de3e06d1e | subsection | 5 | 20 | Experimental set-up and methods | The
region of interest (see Fig. REF ) is lit from above
in order to directly relate light intensity as measured by the camera
to the absorption of light by dye, hence to dye concentration. We
choose the acquisition frequency of the camera to be a multiple of the
stirring frequency. A careful calibration of the respons... | {
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"end": 443,
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"raw": "E. Gouillart, Ph.D. thesis, “A study of chaotic mixing in rod-stirring devices, in closed and open flows,” Université Pierre et Marie Curie, Paris, 2007.",
"source_ref_id": "c062f7d8b3614860ef... | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
"Emmanuelle Gouillart",
"Olivier Dauchot",
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f4573f1a576038f04c10506ae5f42130c8ca7e84 | subsection | 6 | 20 | Mixing patterns and their link with the chaotic saddle | In this section, we describe briefly some qualitative features of
mixing patterns in our experiments. In the Stokes (viscous) flow
regime, the presence of the side walls sharply dampens the stirring
flow. We may thus consider the flow as steady and x-independent
outside a mixing region. The typical size of the mixing r... | {
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"raw": "J. M. Ottino, The Kinematics of Mixing: Stretching, Chaos, and Transport (Cambridge University Press, Cambridge, U.K., 1989).",
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... | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
"Emmanuelle Gouillart",
"Olivier Dauchot",
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0e888b551ffc4fcba98a46cb9b91c6983043a6e5 | subsection | 7 | 20 | Mixing patterns and their link with the chaotic saddle | We shall see that butterfly protocols indeed
give rise to permanent patterns, whereas the spatial distribution of dye
keeps evolving in the breaststroke case. We shall also explain the origin
of such a difference.Important differences between mixing dynamics in the two protocols may
already be inferred from direct visu... | {
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"raw": "T. Tél, in Directions in Chaos, edited by H. B. Lin (World Scientific, Singapore, 1990), Vol. 3, pp. 149–221.",
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"start": 161... | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
"Emmanuelle Gouillart",
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1c0850abb926c3473f009181a4d59cef554b8e17 | subsection | 8 | 20 | Butterfly protocol: onset of a strange
eigenmode | In this section, we consider the evolution of the statistical properties
of the concentration field in the butterfly protocol, and we show that
the visual observation of a concentration eigenmode is confirmed quantitatively.
[Figure: (Previous page) Butterfly protocol: (a) Rectangular region of themixing pattern where ... | {
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"raw": "C. Jung, T. Tél, and E. Ziemniak, “Application of scattering chaos to particle transport in a hydrodynamical flow,” Chaos 3, 555 (1993).",
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"Emmanuelle Gouillart",
"Olivier Dauchot",
"Jean-Luc Thiffeault",
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59c4c1d27bca06f1cd069713da09df7c241991d0 | subsection | 9 | 20 | Butterfly protocol: onset of a strange
eigenmode | REF (e)) converges rapidly to unity, indicating a
persistent pattern. This means that after a short transient phase the
evolution of the concentration field is self-similar, and is therefore
described by the exponential decay of its mean:\mathbf {x}, t) = \langle C \rangle (t) \times \tilde{C}(\mathbf {x}) = C_\infty \... | {
"cite_spans": []
} | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
"Emmanuelle Gouillart",
"Olivier Dauchot",
"Jean-Luc Thiffeault",
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04ee8a2fd26271a141ff80bd87003f9de0b410dd | subsection | 10 | 20 | An open-flow baker's map model | Since Pierrehumbert drew attention to invariant patterns and strange
eigenmodes , much work has been devoted to their
characterization in closed flows. The mean concentration is conserved in
a closed geometry, so the evolution of the eigenmode corresponds to an
exponential decay of fluctuations around the mean by avera... | {
"cite_spans": [
{
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"raw": "R. T. Pierrehumbert, “Tracer microstructure in the large-eddy dominated regime,” Chaos Solitons Fractals 4, 1091 (1994).",
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"s... | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
"Emmanuelle Gouillart",
"Olivier Dauchot",
"Jean-Luc Thiffeault",
"Stéphane Roux"
] | [
"nlin.CD"
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a447b2274b6818bc0ea6c4b3597226c7a1102b16 | subsection | 11 | 20 | An open-flow baker's map model | Hence, in the following calculation
we limit ourselves to a one-dimensional version of the baker's map.Inside the unit interval, the baker's map g readsg: x \mapsto g_1(x) \cup g_2(x),\qquad 0\le x\le 1,whereg_1(x) = U+ \gamma x\,;\qquad g_2(x) = U+ \gamma + (1-\gamma )xand the union (\cup ) symbol in (REF ) means
that... | {
"cite_spans": [
{
"arxiv_id": "",
"doi": "",
"end": 1548,
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"raw": "T. Tél, J. Vollmer, and W. Breymann, “Transient chaos: the origin of transport in driven systems,” Europhys. Lett. 35, 659 (1996).",
"source_ref_id": "73c3488942823ea68e7664df33d65e8017fd9b6f... | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
"Emmanuelle Gouillart",
"Olivier Dauchot",
"Jean-Luc Thiffeault",
"Stéphane Roux"
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"nlin.CD"
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092bee934fa06c3559cf04a659bea89d8e5e6238 | subsection | 12 | 20 | An open-flow baker's map model | Moreover, concentration histograms collapse onto a
single curve when the concentration is rescaled by its mean value
(Fig. REF (b)). The map therefore reproduces well the
salient features observed in the physical flow. | {
"cite_spans": []
} | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
"Emmanuelle Gouillart",
"Olivier Dauchot",
"Jean-Luc Thiffeault",
"Stéphane Roux"
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8161743e7c22979479c13d8406903948d1cc0877 | subsection | 13 | 20 | Symbolic dynamics of the open-flow baker's map | We now exploit the simplicity of the map to gain more insight into the
structure of the asymptotic concentration pattern, and to describe its
evolution with time. Periodic points of the chaotic saddle play a
special role in the concentration profile, as they form the backbone
of the profile. Some iterates of dye partic... | {
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{
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"raw": "T. Tél, G. Károlyi, A. Péntek, I. Scheuring, Z. Toroczkai, C. Grebogi, and J. Kadtke, “Chaotic advection, diffusion, and reactions in open flows,” Chaos 10, 89 (2000).",
"source_ref_id": "f12... | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
"Emmanuelle Gouillart",
"Olivier Dauchot",
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0f0d6a6221af41aa377a069d925ee8f0f03df518 | subsection | 14 | 20 | Symbolic dynamics of the open-flow baker's map | Moreover, g_1 compresses both L and R
inside L, whereas g_2 moves a compressed image of L to the
location of R, and advects R downstream. Defining as L_t and
R_t the amount of dye remaining in the two blocks at time t, we
obtain the symbolic dynamics , L_{t+1} &= \gamma \left[L_t + R_t \right], \\
R_{t+1} &= (1-\gamma ... | {
"cite_spans": [
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"raw": "D. Beigie, A. Leonard, and S. Wiggins, “A global study of enhanced stretching and diffusion in chaotic tangles,” Phys. Fluids 3, 1039 (1991).",
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"Olivier Dauchot",
"Jean-Luc Thiffeault",
"Stéphane Roux"
] | [
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350bebcc2250d144d492aa80139f779e17641d9a | subsection | 15 | 20 | Symbolic dynamics of the open-flow baker's map | Neglecting round-off
and truncation errors, we may consider that C measured at time t
represents the total amount of dye inside the whole unit interval at
time t - n, multiplied by the compression factor \Gamma ^{n}, that
is a quantityC(x,t)\simeq \Gamma ^{n}(L_{t - n} + R_{t - n}).In the next period t+1, the value of ... | {
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dfae668f832ded9d5682b2815b9042cee5dedac0 | subsection | 16 | 20 | Deviations from the strange eigenmode | In sections and , we showed the appearance
of a concentration eigenmode for experiments conducted with the butterfly
protocol, where the chaotic saddle is located far from the channel walls,
and we used an open-flow baker's map to provide a simple physical
picture of this evolution. We now report on experiments
where ... | {
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... | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
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51a7b8a346ea13858d115725b75cee35e664c38f | subsection | 17 | 20 | Deviations from the strange eigenmode | In contrast, for butterfly protocols the
mixing pattern rapidly adopts a constant shape.Dye filaments from the initial blob are therefore trapped for long times
in the vicinity of separation points, where they are hardly stretched and
mixed. Unmixed fluid is slowly reinjected along the unstable manifold of
separation p... | {
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... | 10.1063/1.3080680 | 0807.1723 | Open-flow mixing: Experimental evidence for strange eigenmodes | [
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ad848d1d3e5ead61322817e34cac26365d215709 | subsection | 18 | 20 | Conclusions | We have studied the mixing of a dye tracer by chaotic advection in an
open-flow geometry, where a net free-surface flow crosses a limited
stirring region. Our device was designed to be relevant for industrial
applications, but our foremost objective was to classify mixing
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213e77d46d3c6fb1970366b61721a2117881cd7b | subsection | 19 | 20 | Conclusions | It may therefore be tempting to relate the
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36d75686c4f3d84704ab127e24dea43c123990a3 | abstract | 0 | 32 | Abstract | Achieving maximum scientific results from the overwhelming volume of
astronomical data to be acquired over the next few decades will demand novel,
fully automatic methods of data analysis. Artificial intelligence approaches
hold great promise in contributing to this goal. Here we apply neural network
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5860940d36328bbc7ec45a694ed362300089b25a | subsection | 1 | 32 | Introduction | Over the past decade advances in observational technologies, computers and eclipsing binary (EB) analysis codes (e.g., WD code: , , ) have enabled the accumulation of an impressive sample of fundamental stellar data. Careful analysis of EB light curves has produced fundamental stellar properties, tests of stellar evolu... | {
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5be09cc519ff2db8956432dd7354a7c250735e03 | subsection | 2 | 32 | Introduction | We present results of applying the trained ANN to a set of 10,000 synthetic detached EBs, to 50 detached real world binaries from the Catalog and AtLas of Eclipsing Binaries (CALEBCALEB is maintained by D. Bradstreet at Eastern University – see http://caleb.eastern.edu.), and to the set of 2580 OGLE LMC binaries classi... | {
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55728af8c6ab382468a6a3adff39541aaf51e6bc | subsection | 3 | 32 | The EBAI project: concept and implementation | Advances in Artificial Intelligence (AI) and the continued operation of Moore's law that predicts doubling of the processing power every two years have created the opportunity for significant progress in solving the types of problems that are limited by the lack of human capital. A new approach, the Intelligent Data Pi... | {
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5588c23afe0f40c0114338589cfff4cbe226e76f | subsection | 4 | 32 | Artificial Neural Networks | An artificial neural network is a simple construct: it is a stack of interconnected layers (cf. Fig. REF ). Each layer is an array of processing elements called units. These units propagate the signal between layers by weighted connections. The units perform non-linear mapping of input data to output parameters.
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00bc5b5871cad47fe8cdf1bd3848a21c90ac1fe1 | subsection | 5 | 32 | Artificial Neural Networks | For each exemplar we perform forward-propagation and compare the results output by the network with the true ones. We then modify the weights so that the discrepancy between the results is reduced for the whole sample. This iterative procedure is called the training or machine learning phase. It is the only computation... | {
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9b55d1ebf846274f7a11cea5d31030dfe6924316 | subsection | 6 | 32 | Choice of ANN principal parameters | Solving the inverse problem for EBs (determining the set of model parameters that best fit the observations) is notoriously difficult because parameter inter-correlations and degeneracy are inherent to the problem and cannot be avoided. Thus considerable care must be taken when selecting the network's output parameters... | {
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e2b4b8297377d6b12654ecc22e0b21d0fb8bcfb1 | subsection | 7 | 32 | Choice of ANN principal parameters | As consequence, even if we used surface brightness as the network's output parameter, we would still have to assume one of the temperatures and therefore still suffer from systematic effects.
Sum of relative radii.
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0eb927cdddcc6e96c22cf696715d86312bce5ebc | subsection | 8 | 32 | The training data-set | The goal of the EBAI project is to rapidly process large amounts of survey data. If the network is to perform successfully, the training sample has to be representative of those data. Although survey results are impressive because of the sheer number of the observed targets, they lack in accuracy, data diversity (i.e. ... | {
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63d76919cec08cd39a9fce5a306558b1d1dcce05 | subsection | 9 | 32 | The training data-set | Thus, \alpha follows a gaussian distribution function \mathcal {N}(1.0, 0.2); \beta is sampled uniformly between 0.01 and 0.5, with the ratio of fractional radii distributed by \mathcal {N}(1.0,1.3); \gamma and \delta follow an exponential distribution \mathcal {E}(0,0.05) in e and a uniform distribution in \omega ; fi... | {
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c7fc28f365840d7d004527b32de25caca242216f | subsection | 10 | 32 | Fitting a smooth curve to observed data | The network expects its input to be given at 200 equidistant phases ranging from -0.5 to 0.5, with phase 0 corresponding to the primary (deeper) minimum. To achieve this, the observed data points must be represented by a smooth analytic function that can later be sampled in equidistant phase points. In the special circ... | {
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b4598e0b0cc84c39f91995950e0c297cee07aa28 | subsection | 11 | 32 | ANN sensitivity to light levels | The generated exemplar light curve fluxes are normalized to the sum of both components' passband luminosities per steradian's worth of area, namely f_\mathrm {norm} = 1 \equiv (L_1+L_2)/4\pi , which assigns unity flux to spherical stars of the given luminosity. Thus, the quarter-phase flux will be unity for well detach... | {
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f543a099eeeaa6a63fb9a8a83aecb3b34c5a6b1f | subsection | 12 | 32 | Selection of the optimal ANN topology | Three-layer back-propagation neural networks are well known for their robustness and applicability on a wide range of computational problems . EBs proved to be no exception: tests with two or more hidden layers had shown that there is no obvious benefit for convergence stability. The real challenge was to determine the... | {
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2d890ddbabb03da6013f64ff51eb4e83e783397a | subsection | 13 | 32 | ANN performance and results | The principal benefit of ANNs is speed; a trained network typically takes seconds on an average computer to process even the largest EB databases. However, the most important question is the reliability of the parameters reproduced by the network. After training the network with 33,235 exemplars, it was tested on a dis... | {
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50ccbabd39fc6e09223d5d91c74364add4f82e46 | subsection | 15 | 32 | Network training | Fig. REF depicts the transformation matrices from input to hidden (I\rightarrow H) layer (left), and from hidden to output (H\rightarrow O) layer (right). The I\rightarrow H matrix determines general mapping properties and projects eclipse patterns clearly; it does not change substantially after the first 10000 iterati... | {
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57d2a387ce974cd04f68c2eab257e14c87fbbece | subsection | 16 | 32 | Network training | \rho _1+\rho _2.
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f0883d8ff864b9ba9135a3fd901aaef12ea6ff27 | subsection | 17 | 32 | Test 1: Synthetic sample of 10,000 EBs | As a first test we evaluated the ANN's performance on a sample of 10,000 detached EB light curves distinct from the training set. The test sample was created using the same method as the training sample, following the same probability distribution functions for parameter values (cf. Fig. REF ) and adding variable amoun... | {
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108e2aba3a27aa08e06fe47fb113c382017a8c9d | subsection | 18 | 32 | Test 2: 50 real-world stars from the CALEB database | Further testing of our approach to automated light curve solution – using a trained ANN followed by optional differential corrections – on real-world detached binaries from the CALEB database. Manual inspection of 59 candidate light curves eliminated 9 as either semi-detached or overcontact, leaving 50 test binaries. O... | {
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9bd62e7331bdccbac1afb6d1bd05572001749d06 | subsection | 19 | 32 | Test 2: 50 real-world stars from the CALEB database | Interestingly, for 7 of these systems the published parameters were discrepant with the results here, which suggests an additional benefit to a uniformly-based automated analysis.lccccccccccccccc
Comparison between CALEB values of parameters (\alpha _C through \epsilon _C), ANN values of parameters (\alpha _N throug... | {
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78d4fa97807b9495c981ab45956a1118a8dbf1d1 | subsection | 20 | 32 | Test 2: 50 real-world stars from the CALEB database | Comparing ANN results against published solutions cannot be done rigorously since, as stated previously, there are systematic discrepancies in the published data; inspecting Table REF and LCs given in Appendix reassures that the network, powered by DC, was capable of getting probable parameters for 50 out of 50 CALEB t... | {
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9fe67f76a00b9fbf734ed7f2ae82d2cb96c977d4 | subsection | 21 | 32 | Application: 2580 stars from OGLE detached EB catalog | published a catalog of 2580 detached EBs detected in a 4.6 square degree area of the central parts of the Large Magellanic Cloud (LMC) which includes photometric data collected during the OGLE-2 microlensing search from 1997 to 2000. The sample consists of 2681 entries due to field overlap. The sample was previously us... | {
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9c04bdb7423724f8c6f872553fad522a3f7759c7 | subsection | 22 | 32 | Application: 2580 stars from OGLE detached EB catalog | Either way this result merits further study.The obtained parameters are not final. The next step would be to feed the ANN results into the light curve solver, similar to what was done for the CALEB data presented in Section REF . Since this paper focuses on the performance of the ANN tier alone, we defer a more thoroug... | {
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171e70fe59d62a5d4d84c122ee8cffec3de0f623 | subsection | 23 | 32 | Inferential science | EB parameters gathered from large surveys can yield statistical insight into the physics governing their distributions. Since our tests of ANNs are shown to provide statistically viable results, the question is what scientific results can we extract from the sample. Even in the absence of thorough analysis with heurist... | {
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64934d9245593ebca4e5d0ca98bdbf2ec3664133 | subsection | 24 | 32 | Inferential science | The values of \chi ^2 are computed by feeding the ANN-derived parameters to PHOEBE, computing the corresponding synthetic curve, scaling it vertically to match the input curve and computing the residuals. The solid line represents the exponential function fit to the 3\sigma -1\sigma boundary, where all points were take... | {
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7bd19e477729fa6648a4d6cd58f962d38e611a9c | subsection | 25 | 32 | Discussion | The EBAI project is motivated by the goal of maximizing the scientific output resulting from the analysis of the future fire-hose of binary star data. For this, we are committed to the application of a rigorous physical model (here, the WD model) that encompasses the complete range of binary star configurations. Moreov... | {
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657686602803097026e2da4854cbd32761e3fd54 | subsection | 26 | 32 | Conclusion | ANNs have proved successful in problems of classification, real-time control, data mining and many other tasks in a variety of scientific and technical applications. This paper demonstrates their utility in parameter estimation for detached binaries, even in the face of parameter degeneracy, the correlation of certain ... | {
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a6356629e3f14d0f99962a4170412b2adabca0ff | subsection | 27 | 32 | Conclusion | Systems with large proximity effects which are fully treated in the WD model will be discussed in a subsequent paper. We will thus be able to apply ANNs in a unified, automated approach to provide starting solutions for eclipsing binary light curves of all classes.This research is supported by NSF/RUI Grant No. AST-05-... | {
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aef5a9ba457e7251d5b9d9bb1bb0979f322ec67d | subsection | 28 | 32 | Polyfit algorithm - details | In Section REF we introduced a light curve fitting algorithm polyfit: a polynomial chain fitter. In this appendix we provide a formal description and comment on the implementation details. The polyfit algorithm fits a polynomial chain \mathcal {P}(x) of piecewise smooth n-th order polynomials connected at the given set... | {
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25bfb8800fe619d48d52e1b1e74a722fadb537c4 | subsection | 29 | 32 | Polyfit algorithm - details | Given the last interval I_N = [x_N, x_1), where x_1 is aliased (x_1 \mapsto x_1+1.0), do the n-th order polynomial least squares fit through data points on that interval:
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d26f076a8d1017f242701b2a3b741d5e25f83d02 | subsection | 30 | 32 | Polyfit algorithm - details | The final \chi ^2_L will correspond to the set of knots x_k that best matches the data.There are some subtleties of the algorithm that had to be incorporated for our particular application:a)
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c098e26b123d022c707a837bfc50c8c61d3a3347 | subsection | 31 | 32 | Network fits to CALEB light curves | In Section REF we submitted 50 real-world EBs from the CALEB database to the ANN. Since published model parameters did not always match the data exactly, direct comparison of the results yielded by the network suffers from systematics. As explained in the main part of the paper, parameters obtained from the ANN were us... | {
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} | 10.1086/591783 | 0807.1724 | Artificial Intelligence Approach to the Determination of Physical
Properties of Eclipsing Binaries. I. The EBAI Project | [
"A. Prsa",
"E. F. Guinan",
"E. J. Devinney",
"M. DeGeorge",
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"J. M. Giammarco",
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4d9a3cc1025ceae2b8c8a1b65935b866370d5993 | abstract | 0 | 8 | Abstract | Single-photon sources (SPSs) are mainly characterized by the minimum value of
their second-order coherence function, viz. their $g^{(2)}$ function. A precise
measurement of $g^{(2)}$ may, however, require high time-resolution devices, in
whose absence, only time-averaged measurements are accessible. These
time-averaged... | {
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} | 10.1103/PhysRevA.79.035801 | 0807.1725 | Coherence measures for heralded single-photon sources | [
"E. Bocquillon",
"C. Couteau",
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"R. Laflamme",
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a90277a5d968b316482d07a42404b99fe9643ce2 | subsection | 1 | 8 | Body | Coherence measures for heralded single-photon sourcesE. Bocquillon
Institute for Quantum Computing and Department of Physics and Astronomy,University of Waterloo, 200 University Ave W., Waterloo, ON, Canada N2L 3G1
Ecole Normale Supérieure, 45, rue d'Ulm, 75230 Paris, France
C. Couteau
Institute for Quantum Computing a... | {
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} | 10.1103/PhysRevA.79.035801 | 0807.1725 | Coherence measures for heralded single-photon sources | [
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814941baba91ad612124d1713c17c26296324532 | subsection | 3 | 8 | Body | Bandpass filters block background light from entering the multi-mode fibers that couple the light to the single-photon detectors.]The first coherence measure studied here is the temporal correlation between signal and idler beams, as a measure of reliability of our heralding mechanism, and is defined as followswhere \h... | {
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3193a30419cd77368f43ae672f38ae6afb1ca467 | subsection | 4 | 8 | Body | We can then write the observed value for N_{si} (\tau ) in terms of P_{si}(\tau ) in the following way whereis the coincidence rate for detecting a signal photon at time t+\tau and an idler photon at time t, where u(t) = 1/(2 \tau _d) if |t|\le \tau _d, and zero otherwise.
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811c92fa90e295b63f5cde332e0383530964c53b | subsection | 5 | 8 | Body | We can show that if we allow for infinitely high time resolutions this method provides us with the correct result . The post-measurement averaging, for any operator \hat{X}, will then be given byThe conditional coherence function in Eq. (REF ) can then be written as followswhere, using the quantum version of the Gaussi... | {
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061f7d640541193ab0f165b6a0bbf09f700ac429 | subsection | 6 | 8 | Body | Here, we measure a time-averaged version of the coherence function by approximating P_{si}(\tau ) with N_{si}(\tau ) as before and P_{si}^{(2)}(0,\tau ,0) with N_{si}^{(2)}(\tau ), the count rate for triple coincidences of an idler photodetection event at t_i =0, and two signal photodetection events at t_1 \in [-\tau _... | {
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4345c39a77242346b25947c1e90ea32176105fa3 | subsection | 7 | 8 | Body | Our theory is well capable of reproducing our experimental results, which demonstrated a high-quality source of sub-picosecond single photons. It also allowed us to study the impacts of the chosen coincidence window, the down-conversion parameters, and the resolution of photodetectors on the outcome. Such analysis enab... | {
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} | 10.1103/PhysRevA.79.035801 | 0807.1725 | Coherence measures for heralded single-photon sources | [
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6105d147aeeccdaa1a952f95f9c3e28b401f3d7b | abstract | 0 | 30 | Abstract | We present results from a low resolution (R~300) near-infrared spectroscopic
variability survey of actively accreting T Tauri stars (TTS) in the
Taurus-Auriga star forming region. Paschen and Brackett series H I
recombination lines were detected in 73 spectra of 15 classical T Tauri
systems. The values of the Pan/PaB, ... | {
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} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
"Jeffrey S. Bary",
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"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
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16b03df64bad5aac84daddebca693f05712efaf0 | subsection | 1 | 30 | Introduction | In the decades since their discovery, photometric variability continues to be a defining characteristic of T Tauri stars (TTS) and has
been observed at most wavelengths with timescales as short as
hours , . In addition to the widely studied photometric variations of TTS, astronomers have begun, more recently, to probe ... | {
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53e50818726b898aa1686f41c31ebdcb96456f74 | subsection | 2 | 30 | Introduction | These infrared H i lines, which possess lower opacities relative to the Balmer series, `conspicuously' lack the blue-shifted absorption features present in
H\alpha and H\beta profiles . The infrared lines
also appear to correlate with the mass accretion rates
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448fd0bbc40865d52c575e11c9599b580cf0cb27 | subsection | 3 | 30 | Introduction | This study suggested that the gas temperatures predicted by
were too low to produce the observed line luminosities
for the \dot{M} values considered. These temperatures agree with
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623025b728fd15b257edd848092bf919ebf59486 | subsection | 4 | 30 | Observations | Multi-epoch spectroscopic observations were made of 16 cTTS in the Taurus-Auriga star forming region. The spectra were acquired using CorMass (Cornell-Massachusetts), a cross-dispersed low resolution (R \sim 300) spectrometer with continuous coverage from 0.8 to 2.5 \mu m , with the 1.8-m Vatican Advanced Technology T... | {
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ebba7a96397c37865b53e0e7de6469779d927d0b | subsection | 5 | 30 | Observations | The fluxes were then dereddened using A_{\rm V} values from , , and and a standard A_\lambda \sim \lambda ^{-1.84} extinction law adopted from .
[Figure: As an example of the data collected for the multi-epoch survey, seven of the spectra obtained for the source DR Tau are presented above. Each spectrum contains mult... | {
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c31b9438b57f744a4f67d9f594c2d846db605ee8 | subsection | 6 | 30 | Analysis of H I Line Ratios | The line fluxes for nine Paschen (Pa\beta , \gamma , \delta , 8, 9, 10, 11, 12, and 14) and eight Brackett series (Br\gamma , 10, 11, 12, 13, 14, 15, and 16) lines were measured. These H i line fluxesThe large width of the CorMass slit would enable us to very accurately flux calibrate the spectra under photometric obse... | {
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} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
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c78537f91fb580907142df200cedd2730568f70f | subsection | 7 | 30 | Calculating H I Line Ratios | Figure 2 shows the dereddened line fluxes, including observational uncertainties, for Pan_{up} to Pa\beta and Brn_{up} to Br\gamma . Only emission lines measured to be 3\sigma detections or better are plotted and only these line are used in this analysis. Seventy-three of the 104 spectra have at least one useful ratio,... | {
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} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
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b4ee71d98ad1c10a7b0844877894e3d92fb76a90 | subsection | 8 | 30 | Calculating H I Line Ratios | 2 — Continued
[Figure: For each of the 73 spectra with detectable Pa\beta and Pa\gamma emission features, we plot the values of the Pa\beta equivalent widths versus the values of the Pa\gamma /Pa\beta line flux ratios. Sources for which we have six or more different epochs of observations have been color coded. The dar... | {
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} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
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"Dawn E. Peterson",
"Matthew J. Nelson"
] | [
"astro-ph"
] | 2,008 | en | Physics | [
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a199e14a9172447ab83130b7ea768c8e58e48770 | subsection | 9 | 30 | Calculating H I Line Ratios | Star
Epoch
Pa\beta
Pa\gamma /Pa\beta(JD - 2450000)
EW(Å)
flux ratioBPTau
2976.8 -5.67 \pm 0.91 1.00 \pm 0.362977.8 -6.86 \pm 0.83 1.01 \pm 0.352986.7 -8.37 \pm 0.73 1.11 \pm 0.212986.9 -9.2 \pm 1.1 0.77 \pm 0.202987.7 -6.54 \pm 0.84 0.96 \pm 0.262988.7 -9.77 \pm 0.78 0.93 \pm 0.162989.6 -8.1 \pm 1.1 0.96 \pm 0.28... | {
"cite_spans": []
} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
"Jeffrey S. Bary",
"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
] | [
"astro-ph"
] | 2,008 | en | Physics | [
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ad92efa7c2e60a9ce3e959efa80150557427a835 | subsection | 10 | 30 | Case B | The determination of the electron cascade and the population densities of the energy levels in recombining hydrogenic atoms is a well-studied problem that, historically, has been divided into two distinct Cases, A and B . Case A applies to a gas for which every transition in the hydrogen atom is optically thin such tha... | {
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"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
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341a6ff94998cc3d58512f38a9a020e5e2128087 | subsection | 11 | 30 | Pa | A Fortran program provided by , and accompanied by the necessary data files (on-line at http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=VI/64) was used to produce models of the Paschen and Brackett decrements as well as the line ratios of Br\gamma to Pan_{up} for a grid of 130 different temperature and electron densi... | {
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"Jeffrey S. Bary",
"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
] | [
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] | 2,008 | en | Physics | [
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a48fd698b477d0625a89727789415f546ce556db | subsection | 12 | 30 | Pa | In contrast, the temperature is poorly constrained by the Pan_{up} transitions with the lower and higher n_{up}-values.Figure 5 contains the line ratio curve for the observed Brackett series features using Br\gamma as the reference transition. Overplotted are four Case B model fits, all with a density of n_{\rm e} = 10... | {
"cite_spans": []
} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
"Jeffrey S. Bary",
"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
] | [
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7cc829df8e9e2ada79f83bc209b6df91d6326980 | subsection | 13 | 30 | Pa | However, for the line ratios with the largest Pan_{\rm up} states, the models with the same temperature and different densities are quite distinct from one another, clearly distinguishing the model that most closely matches the data. As a result, the Br\gamma to Pan_{up} line ratios place a strong constraint on the n_{... | {
"cite_spans": []
} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
"Jeffrey S. Bary",
"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
] | [
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3b3144044afd539eaec3acb588c7b746c326a30a | subsection | 14 | 30 | Body | In this section, the reduced \chi ^2-values for each of the 130
temperature and electron density dependent Case B models calculated
for the Brackett series and the Br\gamma /Pan line ratios are
combined to determine which models are the best fits to the combined
dataNote that the \chi ^2-values for the Paschen series
m... | {
"cite_spans": []
} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
"Jeffrey S. Bary",
"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
] | [
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e6c257148e5bb6b954617e1cefcd001ea96e4b9b | subsection | 15 | 30 | Comparison to Optically Thick and Thin LTE Cases | In this section, we compare the observed line ratios to those predicted for gas at a variety of temperatures in both the optically thick (\tau \gg 1) or thin (\tau \ll 1) LTE regimes. | {
"cite_spans": []
} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
"Jeffrey S. Bary",
"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
] | [
"astro-ph"
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3e337f4e296a142a0eb7ba62c6368cc7bc656316 | subsection | 16 | 30 | Optically Thick Case | In general, for optically thick gas in LTE, the intensities of all lines approach the value for a blackbody of a single temperature. Assuming that the line widths are proportional to the wavelength of the line (as expected for Doppler broadening), the line flux ratios are determined by{F_1 \over F_2} = {{\lambda _1 B_\... | {
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"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
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0066afb0ca4f258b7d2a002fcac6fc34009acdd8 | subsection | 17 | 30 | Optically Thin Case | We next consider the optically thin LTE case, where the line flux ratios only depend on the relative population densities of the atoms in the upper n-levels, the associated Einstein A-values, and the wavelengths of the transitions. For a gas in LTE, the level populations follow a Boltzmann distribution, which was used ... | {
"cite_spans": []
} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
"Jeffrey S. Bary",
"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
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5edfc041b8e5f0b39072cc801402fdfa9b9a0523 | subsection | 18 | 30 | Br | Upon inspection of Figures 6 and 8, we note that the Case B models and the optically thin LTE case at different temperatures, predict nearly the same value for the Br\gamma /Pa\delta line ratio. This ratio is unique amongst the others in this series because the electrons share the same n_{up}-level (n_{up} = 7). Thus t... | {
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"Michael F. Skrutskie",
"John C. Wilson",
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9259f68404641e42c3ba2170e7246520a5b8ce08 | subsection | 19 | 30 | Discussion | The Case B determination of gas temperature and electron density of the emitting H i gas is completely independent of any assumptions about where the emission arises (e.g., in a wind, magnetically-channeled accretion flow, or disk). In this section, we discuss the T and n_{\rm e} ranges constrained by the Case B analys... | {
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} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
"Jeffrey S. Bary",
"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
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7e84e8027a1dabcf825a04caa8736283e9b0cdb3 | subsection | 20 | 30 | Accretion Flow Density | For a fiducial accretion rate of \dot{M} = 10^{-7} M_\odot yr^{-1},
magnetospheric accretion models predict a hydrogen density in the
accretion flow to be \sim 10^{12}-10^{13} cm^{-3} , , . For the ionization fractions calculated by
, \sim 10^{-2}-10^{-3}, the range of electron densities for the
accreting gas is expect... | {
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"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
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d2b31c3db94094e4d332c1ccd59a496873c3edb6 | subsection | 21 | 30 | Accretion Flow Density | Differences in \dot{M} and the gas density may impact the recombination timescale and the ionization faction in such a way as to approximately regulate the electron density in the accreting flow.Of course, it is unclear whether either of the above processes are responsible
for the small range of electron densities favo... | {
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} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
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"Dawn E. Peterson",
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b07737352cc3ade7f99c0ba74d2650de8d92f9dc | subsection | 22 | 30 | Accretion Flow Temperature and Luminosity | The preferred values of the gas temperatures derived from the Case B analysis fall
in the range of T 2000 K and are substantially lower than the
range of temperatures predicted by the magnetospheric accretion models of
6000 T 12000 K , . In the models of , the gas temperature was a tunable
parameter. The “optimal” t... | {
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f777a34a3e4d341d9e41f0193cff6a7b672dae67 | subsection | 23 | 30 | Cooling Time of Gas in the Accretion Flow | In order to gain more insight into the thermal structure of the accretion flow, in this section, we estimate the radiative cooling time of the gas, \tau _{\rm cool}. found that the total radiated luminosity of the accretion flow, L_{\rm af}, is comprised primarily of hydrogen continuum emission (75%), plus a significan... | {
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e9b3d607ab660f1341c8c9437188f9a3a1b91d93 | subsection | 24 | 30 | Cooling Time of Gas in the Accretion Flow | This will be true, even for the higher temperatures predicted by magnetospheric accretion models.In order to simultaneously explain the large observed luminosities and low temperatures favored by the Case B analysis, the accretion flow radiation models need to be improved. In order to power the emission, additional hea... | {
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ae4d6efb84701126726cf54b7aab08a96a84db03 | subsection | 25 | 30 | How Important is Ionizing Radiation? | The models of and included an
ionizing source of photons with a luminosity of \sim 10^{28} erg
s^{-1} (shortward of 912 Å). Since this is not capable of
powering the observed line luminosities, it is not surprising that
these works favored temperatures on the order of \sim 10^4 K, where thermal
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93d69c63412291a748db5c5c0726dd39e8f13268 | subsection | 26 | 30 | Summary and Conclusions | In this multi-epoch spectroscopic survey, the line ratios from 17 Paschen and Brackett H i emission features were measured from a total of 73 spectra of 15 actively accreting cTTS. The values of the line fluxes measured for the strongest features (e.g., Pa\beta ) over the entire sample span almost two orders of magnitu... | {
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"Jeffrey S. Bary",
"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
] | [
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0b968ea4afc8ec357d7328588dfce557f63ae56b | subsection | 27 | 30 | Level Populations and Optical Depth | The measured values for the H i line ratios and those expected for both the optically thick and thin LTE cases for any temperature were not in agreement. This result is evidence that the n, l-level populations of the H i gas are not in LTE. On the other hand, the observed ratios were statistically well-fit by
the predi... | {
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} | 10.1086/591487 | 0807.1727 | Physical Conditions of Accreting Gas in T Tauri Star Systems | [
"Jeffrey S. Bary",
"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
] | [
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50024f03d982c62062ffb6f98652e1460dd219c1 | subsection | 28 | 30 | Density | The observed line ratios are statistically well-fit by Case B models
with an electron density of n_{\rm e} = 10^{10} cm^{-3} (§REF ). Furthermore, electron densities of ~10^{11} cm^{-3}
and ~10^{9} cm^{-3} are statistically ruled out at the
99% level or higher (depending on the temperature). Thus it appears
that the ra... | {
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"Sean P. Matt",
"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
] | [
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632d0a0320d9d594fe93f83e28c41eb5d855c18f | subsection | 29 | 30 | Temperature | The Case B statistical analysis rules out electron temperatures of T
\ge 5000 K for the emitting H i gas, at the 99.9% level
(§REF ). Temperatures of 2000 K are favored,
and temperatures as low as a few hundred Kelvin cannot be
ruled out. These temperatures are well below the predictions of the
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"Michael F. Skrutskie",
"John C. Wilson",
"Dawn E. Peterson",
"Matthew J. Nelson"
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2d51ab705bd1bd2bef03147df56c0a5d0985a6c9 | abstract | 0 | 9 | Abstract | Aims: Molecular emission lines originating in the nuclei of luminous
infra-red galaxies are used to determine the physical properties of the nuclear
ISM in these systems.
Methods: A large observational database of molecular emission lines is
compared with model predictions that include heating by UV and X-ray radiatio... | {
"cite_spans": []
} | 10.1051/0004-6361:200810327 | 0807.1728 | Mechanical feedback in the molecular ISM of luminous IR galaxies | [
"A. F. Loenen",
"M. Spaans",
"W. A. Baan",
"R. Meijerink"
] | [
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] | 2,008 | en | Physics | [
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f9588a0839b102a219b4ddb85485e0556d89b299 | subsection | 1 | 9 | Introduction | Dense (n>10^4{\rm cm}^{-3}) molecular gas plays an important
role in the physics of (Ultra-) Luminous Infrared Galaxies. It
provides the materials from which stars are formed and fuels possible
active galactic nuclei. The radiation originating in molecular gas
in the nuclei of these galaxies provides information about ... | {
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{
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"raw": "Hollenbach, D. J. & Tielens, A. G. G. M. 1999, Reviews of Modern Physics, 71, 173",
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{
"arxiv_id... | 10.1051/0004-6361:200810327 | 0807.1728 | Mechanical feedback in the molecular ISM of luminous IR galaxies | [
"A. F. Loenen",
"M. Spaans",
"W. A. Baan",
"R. Meijerink"
] | [
"astro-ph"
] | 2,008 | en | Physics | [
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339ca5f02d2193ab715c60da6cf72e90b0e25b50 | subsection | 2 | 9 | PDR and XDR models | Figure REF shows the HCN, HNC and HCO^+ line ratios
from . To identify the physical processes
that generate the line ratios measured, we compare the data with the
predictions of a large number of PDR and XDR models.
and presented a code
to model one-dimensional PDR and XDR clouds. It takes into account
the various hea... | {
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"arxiv_id":... | 10.1051/0004-6361:200810327 | 0807.1728 | Mechanical feedback in the molecular ISM of luminous IR galaxies | [
"A. F. Loenen",
"M. Spaans",
"W. A. Baan",
"R. Meijerink"
] | [
"astro-ph"
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... |
5bd03905dd77399a50bbab74940fd958675ce3e8 | subsection | 3 | 9 | Mechanical heating | The observed low HNC/HCN ratios could be produced by an enhanced
conversion of HNC into HCN in warm gas. At temperatures higher than
100 K, HNC is converted efficiently into HCN
, . Dense molecular gas temperatures in excess of
100 K have been observed. presented
interferometric maps of NH_3 of the central 500 pc of th... | {
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"A. F. Loenen",
"M. Spaans",
"W. A. Baan",
"R. Meijerink"
] | [
"astro-ph"
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90d01e59f4a0691722d17db2e711da225cb521ad | subsection | 4 | 9 | Mechanical heating | An
explanation for why these high-density systems are not observed is
that the mechanical energies needed to heat the gas are
unavailable (see Sect. ). reported strong HCN emission in the cores
of some Seyfert galaxies (“HCN-enhanced nuclei”, or HENs). Because
of the lack of evidence for a strong nuclear starburst (e.g... | {
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} | 10.1051/0004-6361:200810327 | 0807.1728 | Mechanical feedback in the molecular ISM of luminous IR galaxies | [
"A. F. Loenen",
"M. Spaans",
"W. A. Baan",
"R. Meijerink"
] | [
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dd67df66170e8ea048453dcca5643cee35f93e71 | subsection | 5 | 9 | Sources of mechanical heating | The addition of mechanical heating to PDR clouds provides a
satisfactory means of explaining the observations. However, we need to
identify an available and sufficient source of energy. During the
evolution of a starburst, there are two feedback processes that
potentially provide sufficient mechanical energy to heat de... | {
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{
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} | 10.1051/0004-6361:200810327 | 0807.1728 | Mechanical feedback in the molecular ISM of luminous IR galaxies | [
"A. F. Loenen",
"M. Spaans",
"W. A. Baan",
"R. Meijerink"
] | [
"astro-ph"
] | 2,008 | en | Physics | [
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... |
cb332fd3f7aac04d9d885215b2c103ee5c21f57b | subsection | 6 | 9 | Sources of mechanical heating | The total energy injection
rate needed for the entire starburst region is then:\frac{dE_{\rm SN}}{dt} = \frac{\pi }{6} D_{\rm SB}^3 ~f_{\rm PDR} ~V_{\rm cloud} ~\Gamma _{\rm mech}~{\rm ergs\,s}^{-1}~.By assuming a mechanical energy output of 10^{51} ergs per SN, the SN rate
can then be expressed as:{\rm SN~rate} = \fra... | {
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{
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"doi": "",
"end": 834,
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} | 10.1051/0004-6361:200810327 | 0807.1728 | Mechanical feedback in the molecular ISM of luminous IR galaxies | [
"A. F. Loenen",
"M. Spaans",
"W. A. Baan",
"R. Meijerink"
] | [
"astro-ph"
] | 2,008 | en | Physics | [
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29ed334ac0b6af3000f51a2cd3c03fd46f1b28a0 | subsection | 7 | 9 | Sources of mechanical heating | First of all, SNe are able to inject the energy
on large scales, redistributing the energy amongst the PDRs,
while YSO outflows are only able to heat single clouds. This requires
all stars and surrounding PDR clouds to be at the same (evolutionary)
stage. Also, the time that an ensemble of stars exists in
the phase whe... | {
"cite_spans": []
} | 10.1051/0004-6361:200810327 | 0807.1728 | Mechanical feedback in the molecular ISM of luminous IR galaxies | [
"A. F. Loenen",
"M. Spaans",
"W. A. Baan",
"R. Meijerink"
] | [
"astro-ph"
] | 2,008 | en | Physics | [
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d5fb5424db8d79b7818fb371dff376a8e228841b | subsection | 8 | 9 | Conclusions | Although PDR, XDR or CR chemistry models can explain the general
behavior of the HCN, HNC and HCO^+ line ratios observed in
nearby star-forming galaxies , they cannot
explain the low HNC/HCN line ratios observed in a large
number of systems. The addition of heating by mechanical feedback
provides a solution to this pro... | {
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"doi": "",
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} | 10.1051/0004-6361:200810327 | 0807.1728 | Mechanical feedback in the molecular ISM of luminous IR galaxies | [
"A. F. Loenen",
"M. Spaans",
"W. A. Baan",
"R. Meijerink"
] | [
"astro-ph"
] | 2,008 | en | Physics | [
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a06eeec2c7e8eb6309d9da51b068be425a1ae4ab | abstract | 0 | 39 | Abstract | Global topological defects may account for the large cold spot observed in
the Cosmic Microwave Background. We explore possibilities of constructing
models of supersymmetric F-term hybrid inflation, where the waterfall fields
are globally SU(2)-symmetric. In contrast to the case where SU(2) is gauged,
there arise Golds... | {
"cite_spans": []
} | 10.1088/1475-7516/2008/09/020 | 0807.1729 | Textures and Semi-Local Strings in SUSY Hybrid Inflation | [
"Richard A. Battye",
"Bjorn Garbrecht",
"Apostolos Pilaftsis"
] | [
"hep-ph",
"astro-ph",
"hep-th"
] | 2,008 | en | Physics | [
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b7858cc794c03cda52302b115ce0e63d2fed860a | subsection | 1 | 39 | Introduction | Recent times have seen cosmology enter a precision era. Measurements
of the cosmic microwave background (CMB) have lead to estimates of the
standard 6 cosmological parameters (see, for example, the 5 year
results from WMAP and references therein). Of
particular interest here are the estimates of the amplitude, A_{\rm ... | {
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{
"arxiv_id": "",
"doi": "",
"end": 248,
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"raw": "J. Dunkley et al. [WMAP Collaboration], “Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Likelihoods and Parameters from the WMAP data,” arXiv:0803.0586 [astro-ph].",
"sour... | 10.1088/1475-7516/2008/09/020 | 0807.1729 | Textures and Semi-Local Strings in SUSY Hybrid Inflation | [
"Richard A. Battye",
"Bjorn Garbrecht",
"Apostolos Pilaftsis"
] | [
"hep-ph",
"astro-ph",
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] | 2,008 | en | Physics | [
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e07c1ab09d06bb16dd466f4c711d87242db9b0e7 | subsection | 2 | 39 | Introduction | However, they cannot be stable by Derrick's theorem and hence, once
formed at the phase transition, they unwind. This unwinding process
takes place in a self-similar fashion such that the density of
textures scales relative to the background. The latter has been shown
to be a more general feature of global field models... | {
"cite_spans": [
{
"arxiv_id": "",
"doi": "",
"end": 350,
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"raw": "N. Turok and D. N. Spergel, “Scaling Solution For Cosmological Sigma Models At Large N,” Phys. Rev. Lett. 66, 3093 (1991).",
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... | 10.1088/1475-7516/2008/09/020 | 0807.1729 | Textures and Semi-Local Strings in SUSY Hybrid Inflation | [
"Richard A. Battye",
"Bjorn Garbrecht",
"Apostolos Pilaftsis"
] | [
"hep-ph",
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