cometadata/datacite-rtg-text-other-reclassification-records huggingface dataset:
Time-Variable Jet Ejections from RW Aur A, RY Tau and DG Tau
Creators: name: Takami, Michihiro
name: Guenther, Hans Moritz
name: Schneider, P. Christian
name: Beck, Tracy L.
name: Karr, Jennifer L.
name: Ohyama, Youichi
name: Galvan-Madrid, Roberto
name: Uyama, Taichi
name: White, Marc
name: Grankin, Konstantin
name: Coffey, Deirdre
name: Liu, Chun-Fan
name: Fukagawa, Misato
name: Manset, Nadine
name: Chen, Wen-Ping
name: Pyo, Tae-Soo
name: Shang, Hsien
name: Ray, Thomas P.
name: Otsuka, Masaaki
name: Chou, Mei-Yin
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: We present Gemini-NIFS, VLT-SINFONI and Keck-OSIRIS observations of near-infrared [Fe II] emission associated with the well-studied jets from three active T Tauri stars; RW Aur A, RY Tau and DG Tau taken from 2012-2021. We primarily covered the redshifted jet from RW Aur A, and the blueshifted jets from RY Tau and DG Tau, to investigate long-term time variabilities potentially related to the activities of mass accretion and/or the stellar magnetic fields. All of these jets consist of several moving knots with tangential velocities of 70-240 km s-1, ejected from the star with different velocities and at irregular time intervals. Via comparison with literature, we identify significant differences in tangential velocities for the DG Tau jet between 1985-2008 and 2008-2021. The sizes of the individual knots appear to increase with time, and in turn, their peak brightnesses in the 1.644-micron emission decreased up to a factor of ~30 during the epochs of our observations. A variety of the decay timescales measured in the [Fe II] 1.644 micron emission can be attributed to different pre-shock conditions if the moving knots are unresolved shocks. However, our data do not exclude the possibility that these knots are due to non-uniform density/temperature distributions with another heating mechanism, or in some cases due to stationary shocks without proper motions. Spatially resolved observations of these knots with significantly higher angular resolutions are necessary to better understand their physical nature.
description: 24 pages, 11 figures, 8 tables, accepted for ApJS
Breaking the Chains: Hot Super-Earth systems from migration and disruption of compact resonant chains
Creators: name: Izidoro, Andre
name: Ogihara, Masahiro
name: Raymond, Sean N.
name: Morbidelli, Alessandro
name: Pierens, Arnaud
name: Bitsch, Bertram
name: Cossou, Christophe
name: Hersant, Franck
Publisher: name: arXiv
Year: 2017
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences

description: "Hot super-Earths" (or "Mini-Neptunes") between 1 and 4 times Earth's size with period shorter than 100 days orbit 30-50\% of Sun-like type stars. Their orbital configuration -- measured as the period ratio distribution of adjacent planets in multi-planet systems -- is a strong constraint for formation models. Here we use N-body simulations with synthetic forces from an underlying evolving gaseous disk to model the formation and long-term dynamical evolution of super-Earth systems. While the gas disk is present, planetary embryos grow and migrate inward to form a resonant chain anchored at the inner edge of the disk. These resonant chains are far more compact than the observed super-Earth systems. Once the gas dissipates resonant chains may become dynamically unstable. They undergo a phase of giant impacts that spreads the systems out. Disk turbulence has no measurable effect on the outcome. Our simulations match observations if a small fraction of resonant chains remain stable, while most super-Earths undergo a late dynamical instability. Our statistical analysis restricts the contribution of stable systems to less than $25\%$. Our results also suggest that the large fraction of observed single planet systems does not necessarily imply any dichotomy in the architecture of planetary systems. Finally, we use the low abundance of resonances in Kepler data to argue that, in reality, the survival of resonant chains happens likely only in $\sim 5\%$ of the cases. This leads to a mystery: in our simulations only 50-60\% of resonant chains became unstable whereas at least 75\% (and probably 90-95\%) must be unstable to match observations.
description: Accepted in MNRAS - Kepler dichotomy section substantially updated
Probing dark matter annihilation in the Galaxy with antiprotons and gamma rays
Creators: name: Cuoco, Alessandro
name: Heisig, Jan
name: Korsmeier, Michael
name: Krämer, Michael
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: High Energy Physics - Phenomenology (hep-ph)
subject: FOS: Physical sciences

description: A possible hint of dark matter annihilation has been found in Cuoco, Korsmeier and Krämer (2017) from an analysis of recent cosmic-ray antiproton data from AMS-02 and taking into account cosmic-ray propagation uncertainties by fitting at the same time dark matter and propagation parameters. Here, we extend this analysis to a wider class of annihilation channels. We find consistent hints of a dark matter signal with an annihilation cross-section close to the thermal value and with masses in range between 40 and 130 GeV depending on the annihilation channel. Furthermore, we investigate in how far the possible signal is compatible with the Galactic center gamma-ray excess and recent observation of dwarf satellite galaxies by performing a joint global fit including uncertainties in the dark matter density profile. As an example, we interpret our results in the framework of the Higgs portal model.
description: 12 pages + references, 4 figures, v2: References added, minor changes in presentation, matches journal version
Magnetic field evolution and equilibrium configurations in neutron star cores: the effect of ambipolar diffusion
Creators: name: Castillo, F.
name: Reisenegger, A.
name: Valdivia, J. A.
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences

description: As another step towards understanding the long-term evolution of the magnetic field in neutron stars, we provide the first simulations of ambipolar diffusion in a spherical star. Restricting ourselves to axial symmetry, we consider a charged-particle fluid of protons and electrons carrying the magnetic flux through a motionless, uniform background of neutrons that exerts a collisional drag force on the former. We also ignore the possible impact of beta decays, proton superconductivity, and neutron superfluidity. All initial magnetic field configurations considered are found to evolve on the analytically expected time-scales towards "barotropic equilibria" satisfying the "Grad-Shafranov equation", in which the magnetic force is balanced by the degeneracy pressure gradient, so ambipolar diffusion is choked. These equilibria are so-called "twisted torus" configurations, which include poloidal and toroidal components, the latter restricted to the toroidal volumes in which the poloidal field lines close inside the star. In axial symmetry, they appear to be stable, although they are likely to undergo non-axially symmetric instabilities.
description: MNRAS, accepted
Unruh deWitt probe of late time revival of quantum correlations in Friedmann spacetimes
Creators: name: Dhanuka, Ankit
name: Lochan, Kinjalk
Publisher: name: arXiv
Year: 2022
Subjects: subject: General Relativity and Quantum Cosmology (gr-qc)
subject: FOS: Physical sciences

description: Unruh deWitt detectors are important constructs in studying the dynamics of quantum fields in any geometric background. Curvature also plays an important role in setting up the correlations of a quantum field in a given spacetime. For instance, massless fields are known to have large correlations in de Sitter space as well as in certain class of Friedmann-Robertson-Walker (FRW) universes. However, some of the correlations are secular in nature while some are dynamic and spacetime dependent. An Unruh deWitt detector responds to such divergences differently in different spacetimes. In this work, we study the response rate of Unruh deWitt detectors which interact with quantum fields in FRW spacetimes. We consider both conventionally as well as derivatively coupled Unruh deWitt detectors. Particularly, we consider their interaction with massless scalar fields in FRW spacetimes and nearly massless scalar fields in de Sitter spacetime. We discuss how the term which gives rise to the infrared divergence in the massless limit in de Sitter spacetime manifests itself at the level of the response rate of these Unruh deWitt detectors in a wide class of Friedmann spacetimes. To carry out this study, we use an equivalence between massless scalar fields in FRW spacetimes with massive scalar fields in de Sitter spacetime. Further, we show that while the derivative coupling regulates the divergence appearing in de Sitter spacetime, it does not completely remove them in matter dominated universe. This gives rise to large transitions in the detector which can be used as a probe of setting up of large correlations in late time era of the universe as well. We show that the coupling of hydrogen atoms with gravitational waves takes a form that is similar to derivatively coupled UdW detectors and hence has significant observational implications as a probe of late time revival of quantum correlators.
description: 29 pages, 5 figures
Comparison between Hadamard and canonical bases for in-situ wavefront correction and the effect of ordering in compressive sensing
Creators: name: Scheidt, Dennis
name: Su, Pedro A. Quinto
Publisher: name: arXiv
Year: 2022
Subjects: subject: Image and Video Processing (eess.IV)
subject: Optics (physics.optics)
subject: FOS: Electrical engineering, electronic engineering, information engineering
subject: FOS: Physical sciences

description: In this work we compare the Canonical and Hadamard bases for in-situ wavefront correction of a focused Gaussian beam using a spatial light modulator (SLM). The beam is perturbed with a transparent optical element (sparse) or a random scatterer (both prevent focusing at a single spot). The phase corrections are implemented with different basis sizes ($N=64, 256, 1024, 4096$) and the phase contribution of each basis element is measured with 3 step interferometry. The field is reconstructed from the complete $3N$ measurements and the correction is implemented by projecting the conjugate phase at the SLM. Our experiments show that in general, the Hadamard basis measurements yield better corrections because every element spans the relevant area of the SLM, reducing the noise in the interferograms. % In contrast, the canonical basis has the fundamental limitation that the area of the elements is proportional to $1/N$, and requires dimensions that are compatible with the spatial period of the grating. In the case of the random scatterer, we were only able to get reasonable corrections with the Hadamard basis and the intensity of the corrected spot increased monotonically with $N$, which is consistent with fast random changes in phase over small spatial scales. We also explore compressive sensing with the Hadamard basis and find that the minimum compression ratio needed to achieve corrections with similar quality to those that use the complete measurements depend on the basis ordering. The best results are reached in the case of the Hadamard-Walsh and cake cutting orderings. Surprisingly, in the case of the random scatterer we find that moderate compression ratios on the order of $10-20\%$ ($N=4096$) allow to recover focused spots, although as expected, the maximum intensities increase monotonically with the number of measurements due to the non sparsity of the signal.
description: 8 pages, 5 figures
If dark matter is fuzzy, the first stars form in massive pancakes
Creators: name: Kulkarni, Mihir
name: Visbal, Eli
name: Bryan, Greg L.
name: Li, Xinyu
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences

description: Fuzzy dark matter (FDM) is a proposed modification for the standard cold dark matter (CDM) model motivated by small-scale discrepancies in low-mass galaxies. Composed of ultra-light (mass $\sim 10^{-22}$ eV) axions with kpc-scale de Broglie wavelengths, this is one of a class of candidates that predicts that the first collapsed objects form in relatively massive dark matter halos. This implies that the formation history of the first stars and galaxies would be very different, potentially placing strong constraints on such models. Here we numerically simulate the formation of the first stars in an FDM cosmology, following the collapse in a representative volume all the way down to primordial protostar formation including a primordial non-equilibrium chemical network and cooling for the first time. We find two novel results: first, the large-scale collapse results in a very thin and flat gas "pancake"; second, despite the very different cosmology, this pancake fragments until it forms protostellar objects indistinguishable from those in CDM. Combined, these results indicate that the first generation of stars in this model are also likely to be massive and, because of the sheet morphology, do not self-regulate, resulting in a massive Pop III starburst. We estimate the total number of first stars forming in this extended structure to be $10^4$ over 20 Myr using a simple model to account for the ionizing feedback from the stars, and should be observable with JWST. These predictions provide a potential smoking gun signature of FDM and similar dark matter candidates.
description: 9 pages, 6 figures, Accepted for publication in ApJL
title: Transformation Processes and Kinetics in the Magnesium Phosphate Mineral System
Creators: name: Volkmann, Rebecca
name: Blukis, Roberts
name: Roddatis, Vladimir
name: Schmidt, Christian
name: Benning, Liane G.
Publisher: name: Deutsche Geologische Gesellschaft - Geologische Vereinigung e.V. (DGGV)
Year: 2022

description:
Phosphorous is an important nutrient for all living beings. Together with nitrogen, it is a crucial element for the global agriculture, yet it is a limited natural resource. The mineral struvite (MgNH4PO4·6H2O) occurs in guano deposits, wastewater pipelines, and pathogenic urinary stones. It´s recovery and reutilization as a slow release fertilizer has become a common process in wastewater treatment. However, it´s instability under atmospheric conditions leads to transformation to other phosphate phases, a process that is still poorly understood.

We investigated this transformation by reacting synthetic, μm- and mm-sized struvite crystals at different temperatures in open and closed systems. We monitored the transformation of struvite with time using ex-situ X-ray diffraction (XRD) and processing with Rietveld refinement. Complementary, transformations of mm-sized crystals were investigated by imaging with optical and scanning electron microscopy and by analysis with Raman spectroscopy.

XRD analysis shows that struvite transforms to newberyite (Mg(PO3OH)·3H2O) at room temperature over several weeks by losing water and ammonium. Optical microscopy reveals newberyite as opaque, white or dark brown patches, inside crystals and at crystal sides. At elevated temperatures (37 and 60 °C), struvite predominantly transforms to dittmarite (MgNH4PO4·H2O) with newberyite as minor product, indicating a temperature-driven loss of water that is faster than ammonium loss. The presence of newberyite and dittmarite was confirmed by Raman spectroscopy. Transformation rates of both the open and closed system were evaluated. These findings are important to understand long-term processes that may influence the properties of wastewater-derived struvite as slow-release fertilizer.
Nonlinear flip-flop quantum walks through potential barriers
Creators: name: Passos, F. S.
name: Buarque, A. R. C.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Quantum Physics (quant-ph)
subject: FOS: Physical sciences

description: The dynamics of nonlinear flip-flop quantum walk with amplitude-dependent phase shifts with pertubing potential barrier is investigated. Through the adjustment between uniform local perturbations and a Kerrlike nonlinearity of the medium we find a rich set of dynamic profiles. We will show the existence of different Hadamard quantum walking regimes, including those with mobile soliton-like structures or self-trapped states. The latter is predominant for perturbations with amplitudes that tend to $φ\rightarrow π/2$. In this system, the qubit shows an unusual behavior as we increase the amplitudes of the potential barriers, and displays a monotonic decrease in the self-trapping $φ_c$ with respect to the nonlinear parameter. A chaotic-like regime becomes predominant for intermediate nonlinearity values. Furthermore, we show that by changing the quantum coins ($θ$) a non-trivial dynamic arises, where coins close to Pauli-X drives the system to a regime with predominant soliton-like structures, while the chaotic behavior are restricted to a narrow region in the $χ$-$φ$ plane. We believe that is possible to implement and observe the proprieties of this model in a integrated photonic system.
Resolved Molecular Gas Observations of MaNGA Post-starbursts Reveal a Tumultuous Past
Creators: name: Otter, Justin Atsushi
name: Rowlands, Kate
name: Alatalo, Katherine
name: Leung, Ho-Hin
name: Wild, Vivienne
name: Luo, Yuanze
name: Petric, Andreea O.
name: Sazonova, Elizaveta
name: Stark, David V.
name: Heckman, Timothy
name: Davis, Timothy A.
name: Ellison, Sara
name: French, K. Decker
name: Baker, William
name: Bluck, Asa F. L.
name: Lanz, Lauranne
name: Lin, Lihwai
name: Liu, Charles
name: Cobá, Carlos López
name: Masters, Karen L.
name: Nair, Preethi
name: Pan, Hsi-an
name: Riffel, Rogemar A.
name: Scudder, Jillian M.
name: Smercina, Adam
name: van de Voort, Freeke
name: Weaver, John R.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: Post-starburst galaxies (PSBs) have recently and rapidly quenched their star-formation, thus they are an important way to understand how galaxies transition from star-forming late-types to quiescent early-types. The recent discovery of large cold gas reservoirs in PSBs calls into question the theory that galaxies must lose their gas to become quiescent. Optical Integral Field Spectroscopy (IFS) surveys have revealed two classes of PSBs: central PSBs with central quenching regions and ring PSBs with quenching in their outskirts. We analyze a sample of 13 nearby (z < 0.1) PSBs with spatially resolved optical IFS data from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey and matched resolution Atacama Large (sub-)Millimeter Array (ALMA) observations of $^{12}$CO(1-0). Disturbed stellar kinematics in 7/13 of our PSBs and centrally concentrated molecular gas is consistent with a recent merger for most of our sample. In galaxies without merger evidence, alternate processes may funnel gas inwards and suppress star-formation, which may include outflows, stellar bars, and minor mergers or interactions. The star-formation efficiencies of the post-starburst regions in nearly half our galaxies are suppressed while the gas fractions are consistent with star-forming galaxies. AGN feedback may drive this stabilization, and we observe AGN-consistent emission in the centers of 5/13 galaxies. Finally, our central and ring PSBs have similar properties except the ionized and molecular gas in central PSBs is more disturbed. Overall, the molecular gas in our PSBs tends to be compact and highly disturbed, resulting in concentrated gas reservoirs unable to form stars efficiently.
description: Accepted for publication in The Astrophysical Journal
Spitzer/IRS full spectral modeling to characterize mineralogical properties of silicate dust in heavily obscured AGNs
Creators: name: Tsuchikawa, T.
name: Kaneda, H.
name: Oyabu, S.
name: Kokusho, T.
name: Kobayashi, H.
name: Toba, Y.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: Mid-Infrared (IR) silicate dust bands observed in heavily obscured active galactic nuclei (AGNs) include information on the mineralogical properties of silicate dust. We aim to investigate the mineralogical picture of the circumnuclear region of heavily obscured AGNs to reveal obscured AGN activities through the picture. In our previous study Tsuchikawa et al. (2021), we investigated the properties of silicate dust in heavily obscured AGNs focusing on the mineralogical composition and the crystallinity with Spitzer/IRS 5.3-12 micron spectra. In this study, we model the full-range Spitzer/IRS 5-30 micron spectra of 98 heavily obscured AGNs using a one-dimensional radiative transfer calculation with four dust species in order to evaluate wider ranges of the properties of silicate dust more reliably. Comparing fitting results between four dust models with a different size and porosity, 95 out of the 98 galaxies prefer a porous silicate dust model without micron-sized large grains. The pyroxene mass fraction and the crystallinity are overall consistent with but significantly different from the previous results for the individual galaxies. The pyroxene-poor composition, small dust size and high porosity are similar to newly formed dust around mass-loss stars as seen in our Galaxy, which presumably originates from the recent circumnuclear starburst activity. The high crystallinity on average suggests dust processing induced by AGN activities.
description: 24 pages, 10 figures, accepted for publication in ApJ
How magnetic field and stellar radiative feedback influences the collapse and the stellar mass spectrum of a massive star forming clump
Creators: name: Hennebelle, Patrick
name: Lebreuilly, Ugo
name: Colman, Tine
name: Elia, Davide
name: Fuller, Gary
name: Leurini, Silvia
name: Nony, Thomas
name: Schisano, Eugenio
name: Soler, Juan D.
name: Traficante, Alessio
name: Klessen, Ralf S.
name: Molinari, Sergio
name: Testi, Leonardo
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: In spite of decades of theoretical efforts, the physical origin of the stellar initial mass function (IMF) is still debated. We aim at understanding the influence of various physical processes such as radiative stellar feedback, magnetic field and non-ideal magneto-hydrodynamics on the IMF. We present a series of numerical simulations of collapsing 1000 M$_\odot$ clumps taking into account radiative feedback and magnetic field with spatial resolution down to 1 AU. Both ideal and non-ideal MHD runs are performed and various radiative feedback efficiencies are considered. We also develop analytical models that we confront to the numerical results. The sum of the luminosities produced by the stars in the calculations is computed and it compares well with the bolometric luminosities reported in observations of massive star forming clumps. The temperatures, velocities and densities are also found to be in good agreement with recent observations. The stellar mass spectrum inferred for the simulations is, generally speaking, not strictly universal and in particular varies with magnetic intensity. It is also influenced by the choice of the radiative feedback efficiency. In all simulations, a sharp drop in the stellar distribution is found at about $M_{min} \simeq$ 0.1 M$_\odot$, which is likely a consequence of the adiabatic behaviour induced by dust opacities at high densities. As a consequence, when the combination of magnetic and thermal support is not too large, the mass distribution presents a peak located at 0.3-0.5 M$_\odot$. When magnetic and thermal support are large, the mass distribution is better described by a plateau, i.e. $d N / d \log M \propto M^{-Γ}$, $Γ\simeq 0$. Abridged
description: accepted for publication in A&A
Living on the edge of the Central Molecular Zone: G1.3 is the more likely candidate for gas accretion into the CMZ
Creators: name: Busch, Laura A.
name: Riquelme, Denise
name: Güsten, Rolf
name: Menten, Karl M.
name: Pillai, Thushara G. S.
name: Kauffmann, Jens
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: The 1.3deg (G1.3) and 1.6deg (G1.6) cloud complexes in the Central Molecular Zone (CMZ) of our Galaxy have been proposed to possibly reside at the intersection region of the X1 and X2 orbits for several reasons. This includes the detection of co-spatial low- and high-velocity clouds, high velocity dispersion, high fractional molecular abundances of shock-tracing molecules, and kinetic temperatures that are higher than for usual CMZ clouds. We mapped both cloud complexes in molecular lines in the frequency range from 85 to 475GHz with the IRAM 30m and the APEX 12m telescopes. The kinematic structure of G1.3 reveals an `emission bridge' at intermediate velocities (~150km/s) connecting low-velocity (~100km/s) and high-velocity (~180km/s) gas and an overall fluffy shell-like structure. These may represent observational evidence of cloud-cloud interactions. Low- and high-velocity gas components in G1.6 do not show such evidence of interaction, suggesting that they are spatially separated. We selected three positions in each cloud complex for further analysis. Based on non-LTE modelling of an ensemble of CH3CN lines, we derived kinetic temperatures of 60-100K and H2 volume densities of 10$^4$-10$^5$cm-3 in both complexes. Molecular abundances relative to H2 suggest a similar chemistry of the two clouds, which is moreover similar to that of other GC clouds. We conclude that G1.3 may indeed exhibit signs of cloud-cloud interactions. We propose an interaction of gas that is accreted from the near-side dust lane to the CMZ, with gas pre-existing at this location. Low- and high-velocity components in G1.6 are rather coincidentally observed along the same line of sight. They may be associated with either overshot decelerated gas from the far-side dust line or actual CMZ gas and high-velocity gas moving on a dust lane. These scenarios would be in agreement with numerical simulations.
description: Accepted for publication in A&A
Initial Correlations in Open Quantum Systems: Constructing Linear Dynamical Maps and Master Equations
Creators: name: Colla, Alessandra
name: Neubrand, Niklas
name: Breuer, Heinz-Peter
Publisher: name: arXiv
Year: 2022
Subjects: subject: Quantum Physics (quant-ph)
subject: FOS: Physical sciences

description: We investigate the dynamics of open quantum systems which are initially correlated with their environment. The strategy of our approach is to analyze how given, fixed initial correlations modify the evolution of the open system with respect to the corresponding uncorrelated dynamical behavior with the same fixed initial environmental state, described by a completely positive dynamical map. We show that, for any predetermined initial correlations, one can introduce a linear dynamical map on the space of operators of the open system which acts like the proper dynamical map on the set of physical states and represents its unique linear extension. Furthermore, we demonstrate that this construction leads to a linear, time-local quantum master equation with generalized Lindblad structure involving time-dependent, possibly negative transition rates. Thus, the general non-Markovian dynamics of an open quantum system can be described by means of a time-local master equation even in the case of arbitrary, fixed initial system-environment correlations. We present some illustrative examples and explain the relation of our approach to several other approaches proposed in the literature.
description: 12 pages, 3 figures
Razor-thin dust layers in protoplanetary disks: Limits on the vertical shear instability
Creators: name: Dullemond, C. P.
name: Ziampras, A.
name: Ostertag, D.
name: Dominik, C.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences

description: Context: Recent observations with the Atacama Large Millimeter Array (ALMA) have shown that the large dust aggregates observed at millimeter wavelengths settle to the midplane into a remarkably thin layer. Aims: We intend to find out if the geometric thinness of these layers is evidence against the vertical shear instability (VSI) operating in these disks. Methods: We performed hydrodynamic simulations of a protoplanetary disk with a locally isothermal equation of state, and let the VSI fully develop. We sprinkled dust particles and followed their motion as they got stirred up by the VSI. We determined for which grain size the layer becomes geometrically thin enough to be consistent with ALMA observations. We then verified if, with these grain sizes, it is still possible to generate a moderately optically thick layer at millimeter wavelengths, as observations appear to indicate. Results: We found that even very large dust aggregates with Stokes numbers close to unity get stirred up to relatively large heights above the midplane by the VSI, which is in conflict with the observed geometric thinness. For grains so large that the Stokes number exceeds unity, the layer can be made to remain thin, but we show that it is hard to make dust layers optically thick at ALMA wavelengths (e.g., tau(1.3mm)>=1) with such large dust aggregates. Conclusions: We conclude that protoplanetary disks with geometrically thin midplane dust layers cannot be VSI unstable, at least not down to the disk midplane. Explanations for the inhibition of the VSI include a reduced dust-to-gas ratio of the small dust grains that are responsible for the radiative cooling of the disk. A reduction of small grains by a factor of between 10 and 100 is sufficient to quench the VSI. Such a reduction is plausible in dust growth models, and still consistent with observations at optical and infrared wavelengths.
description: Accepted for publication in Astronomy & Astrophysics
Single-sideband modulator for frequency domain multiplexing of superconducting qubit readout
Creators: name: Chapman, Benjamin J.
name: Rosenthal, Eric I.
name: Kerckhoff, Joseph
name: Vale, Leila R.
name: Hilton, Gene C.
name: Lehnert, K. W.
Publisher: name: arXiv
Year: 2017
Subjects: subject: Quantum Physics (quant-ph)
subject: Superconductivity (cond-mat.supr-con)
subject: FOS: Physical sciences

description: We introduce and experimentally characterize a superconducting single-sideband modulator compatible with cryogenic microwave circuits, and propose its use for frequency domain multiplexing of superconducting qubit readout. The monolithic single-quadrature modulators that comprise the device are formed with purely reactive elements (capacitors and Josephson junction inductors) and require no microwave-frequency control tones. Microwave signals in the 4 to 8 GHz band, with power up to -85 dBm, are converted up or down in frequency by as much as 120 MHz. Spurious harmonics in the device can be suppressed by up to 25 dB for select probe and modulation frequencies.
description: 5 page main text, 6 page supplementary information
A Molecular Gas Ring Hidden in the Sombrero Galaxy
Creators: name: Sutter, Jessica
name: Fadda, Dario
Publisher: name: arXiv
Year: 2022
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences

description: We present Herschel, ALMA, and MUSE observations of the molecular ring of Messier 104, also known as the Sombrero galaxy. These previously unpublished archival data shed new light on the content of the interstellar medium of M104. In particular, molecular hydrogen measured by CO emission and dust measured by far-infrared light are uniformly distributed along the ring. The ionized gas revealed by H$α$ and [CII] emission is distributed in knots along the ring. Despite being classified as an SAa galaxy, M104 displays features typical of early-type galaxies. We therefore compared its [CII] and dust emission to a sample of early-type galaxies observed with Herschel and SOFIA. The [CII]/FIR ratio of M104 is much lower than that of typical star-forming galaxies and is instead much more similar to that of early-type galaxies. By classifying regions using optical emission line diagnostics we also find that regions classified as HII lie closer to star-forming galaxies in the [CII]/FIR diagram than those classified as low-ionization emission regions. The good match between [CII] and H$α$ emission in conjunction with the lack of correlation between CO emission and star formation suggest that there is very limited active star formation along the ring and that most of the [CII] emission is from ionized and neutral atomic gas rather than molecular gas. From the total intensity of the CO line we estimate a molecular hydrogen mass of 0.9$\times10^9$M$_{\odot}$, a value intermediate between those of early type galaxies and the content of the molecular ring of our galaxy.
description: 29 pages, 14 figures, accepted for publication at ApJ
Scattering unitarity with effective dimension-6 operators
Creators: name: Ghosh, Swagata
name: Islam, Rashidul
name: Kundu, Anirban
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Physics - Phenomenology (hep-ph)
subject: FOS: Physical sciences

description: The effects of physics beyond the Standard Model may be parametrized by a set of higher-dimensional operators leading to an effective theory. The introduction of these operators makes the theory nonrenormalizable, and one may reasonably expect a violation of unitarity in $2\to 2$ scattering processes,depending on the values of the Wilson coefficients of the higher dimensional operators. Bounds on these coefficients may be obtained from demanding that there be no such unitarity violation below the scale of the effective theory. We show, at the lowest level, how the new operators affect the scattering amplitudes with longitudinal gauge bosons, scalars, and $t\bar{t}$ in the final state, and find that one may expect a violation of unitarity even at the LHC energies with small values of some of the new Wilson coefficients. For most of the others, such a violation needs large coefficients, indicating nonperturbative physics for the ultraviolet-complete theory, although a proper treatment necessitates the inclusion of even higher-dimensional operators. However, deviations from the Standard Model expectations may be observed with even smaller values for these coefficients. We find that $WW \to WW$, $WW\to ZZ$, and $ZZ\to hh$ scatterings are the best possible channels to probe unitarity violations.
description: 19 pages, 3 figures. The section on results substantially extended. Final version accepted for publication
title: Magma evolution and epithermal ore formation at Conical Seamount, Papua New Guinea
Creators: name: Gautreau, Louis-Maxime
name: Brandl, Philipp A.
name: Hansteen, Thor H.
Publisher: name: Deutsche Geologische Gesellschaft - Geologische Vereinigung e.V. (DGGV)
Year: 2022

description:
The Tabar-Lihir-Tanga-Feni (TLTF) island chain in northeastern Papua New Guinea hosts the world-class Ladolam gold deposit on Lihir island as well as several other Au prospects. Several young seamounts are located around Lihir and were studied in detail by three RV Sonne cruises in 1994, 1998 and 2002. While most of these seamounts are considered barren, Conical Seamount, located southeast of Lihir island, shows evidence for epithermal-style mineralization and has been interpreted as a submarine analogue to the Ladolam deposit. It offers a rare opportunity to study a porphyry-epithermal ore system at a juvenile stage and compare it to a mature system nearby.

In the first phase of our research project, we focus on the igneous system underlying the epithermal ore-forming system at Conical. We study the lavas as well as minerals and glass inclusions to reconstruct melting processes, magma evolution and ore fertility using detailed petrology, in situ geochemistry and thermobaric modelling. Special emphasis is given to volatile as well as trace metal and metalloid contents in bulk rocks, glasses and glass inclusions. Mineral zonations and the compositional diversity of pyroxene-hosted glass inclusions point towards repeated magma recharge and the potential existence of multiple magma stagnation levels. While the high melt oxidation state (∆ log fO2 of +0.5 to +2 relative to FMQ) at Conical is advantageous for the enrichment of chalcophile elements in the evolving melt, high volatile contents may promote early fluid exsolution and the transfer of metals and metalloids into the epithermal system.
The limits of rechargeable spin battery
Creators: name: Yanovsky, A. V.
name: Pyshkin, P. V.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Mesoscale and Nanoscale Physics (cond-mat.mes-hall)
subject: FOS: Physical sciences

description: We discuss how the ideal rechargeable energy accumulator can be made, and what are the limits for solid state energy storage. We show that in theory the spin batteries based on heavy fermions can surpass the chemical ones by energy capacitance. The absence of chemical reactions in spin batteries makes them more stable, also they don't need to be heated in cold conditions. We study how carriers statistics and density of states affect energy capacity of the battery. Also, we discuss hypothetical spin batteries based on neutron stars.
A high resolution ion microscope for cold atoms
Creators: name: Stecker, Markus
name: Schefzyk, Hannah
name: Fortágh, József
name: Günther, Andreas
Publisher: name: arXiv
Year: 2017
Subjects: subject: Atomic Physics (physics.atom-ph)
subject: FOS: Physical sciences

description: We report on an ion-optical system that serves as a microscope for ultracold ground state and Rydberg atoms. The system is designed to achieve a magnification of up to 1000 and a spatial resolution in the 100 nm range, thereby surpassing many standard imaging techniques for cold atoms. The microscope consists of four electrostatic lenses and a microchannel plate in conjunction with a delay line detector in order to achieve single particle sensitivity with high temporal and spatial resolution. We describe the design process of the microscope including ion-optical simulations of the imaging system and characterize aberrations and the resolution limit. Furthermore, we present the experimental realization of the microscope in a cold atom setup and investigate its performance by patterned ionization with a structure size down to 2.7 μm. The microscope meets the requirements for studying various many-body effects, ranging from correlations in cold quantum gases up to Rydberg molecule formation.
description: 11 pages, 11 figures
Probing stellar binary black hole formation in galactic nuclei via the imprint of their center of mass acceleration on their gravitational wave signal
Creators: name: Inayoshi, Kohei
name: Tamanini, Nicola
name: Caprini, Chiara
name: Haiman, Zoltan
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: General Relativity and Quantum Cosmology (gr-qc)
subject: FOS: Physical sciences

description: Multi-frequency gravitational wave (GW) observations are useful probes of the formation processes of coalescing stellar-mass binary black holes (BBHs). We discuss the phase drift in the GW inspiral waveform of the merging BBH caused by its center-of-mass acceleration. The acceleration strongly depends on the location where a BBH forms within a galaxy, allowing observations of the early inspiral phase of LIGO-like BBH mergers by the Laser Interferometer Space Antenna (LISA) to test the formation mechanism. In particular, BBHs formed in dense nuclear star clusters or via compact accretion disks around a nuclear supermassive black hole in active galactic nuclei would suffer strong acceleration, and produce large phase drifts measurable by LISA. The host galaxies of the coalescing BBHs in these scenarios can also be uniquely identified in the LISA error volume, without electromagnetic counterparts. A non-detection of phase drifts would rule out or constrain the contribution of the nuclear formation channels to the stellar-mass BBH population.
description: 8 pages, 4 figures, 1 table, accepted for publication in Physical Review D
Nurrenbern Road wetland hydrologic and hydraulic design
Creators: name: Sollman, Corbin
name: Kollak, Storm
Publisher: name: Unknown
Year: 2018

description: The University of Southern Indiana has expressed interest in the restoration of a wetland located
adjacent to Nurrenbern Road in Southern Vanderburgh County. Once constructed, the wetland will
support research and teaching activities for USI students and faculty in the biology, geology, and
engineering departments. In 2013, a senior design group at USI conducted a comprehensive hydraulic
and hydrologic analysis to evaluate the potential to restore the site into its original wetland condition.
The site was determined to have great potential for restoration. A monitoring program was initiated
consisting of groundwater monitoring wells and a rain gauge. Data was collected over several years. The
site is now being considered as a mitigation site to offset wetland loss in the county. The objective of
this project was to complete the final design, including processing hydrologic data. Key components of
the design include a grade plan, drainage culvert, and a diversion weir. A site survey of the tributary
stream was completed so that the culvert, weir, and grade plan could be accurately modeled and
designed. Two proposed grading plans were designed, including varying elevations in order to promote
biodiversity found in natural wetlands and to encourage accumulation of water within the site. An inline,
V-notch weir structure and a drainage culvert were designed to divert additional water from an onsite
tributary stream into the designed wetland storage area. The results indicate a high likelihood of success
for the proposed mitigation design. A detailed cost analysis was performed for the construction of the
earth work, inline weir, and the drainage culvert.
Searches for Double Beta Decay of $^{134}$Xe with EXO-200
Creators: name: 200 Collaboration
name: Albert, J. B.
name: Anton, G.
name: Badhrees, I.
name: Barbeau, P. S.
name: Bayerlein, R.
name: Beck, D.
name: Belov, V.
name: Breidenbach, M.
name: Brunner, T.
name: Cao, G. F.
name: Cen, W. R.
name: Chambers, C.
name: Cleveland, B.
name: Coon, M.
name: Craycraft, A.
name: Cree, W.
name: Daniels, T.
name: Danilov, M.
name: Daugherty, S. J.
name: Daughhetee, J.
name: Davis, J.
name: Delaquis, S.
name: Der Mesrobian-Kabakian, A.
name: DeVoe, R.
name: Didberidze, T.
name: Dilling, J.
name: Dolgolenko, A.
name: Dolinski, M. J.
name: Fairbank, W.
name: Farine, J.
name: Feyzbakhsh, S.
name: Fierlinger, P.
name: Fudenberg, D.
name: Gornea, R.
name: Graham, K.
name: Gratta, G.
name: Hall, C.
name: Hoessl, J.
name: Hufschmidt, P.
name: Hughes, M.
name: Jamil, A.
name: Jewell, M. J.
name: Johnson, A.
name: Johnston, S.
name: Karelin, A.
name: Kaufman, L. J.
name: Koffas, T.
name: Kravitz, S.
name: Krücken, R.
name: Kuchenkov, A.
name: Kumar, K. S.
name: Lan, Y.
name: Leonard, D. S.
name: Li, S.
name: Licciardi, C.
name: Lin, Y. H.
name: MacLellan, R.
name: Marino, M. G.
name: Michel, T.
name: Mong, B.
name: Moore, D.
name: Murray, K.
name: Nelson, R.
name: Njoya, O.
name: Odian, A.
name: Ostrovskiy, I.
name: Piepke, A.
name: Pocar, A.
name: Retière, F.
name: Rowson, P. C.
name: Russell, J. J.
name: Schubert, A.
name: Sinclair, D.
name: Smith, E.
name: Stekhanov, V.
name: Tarka, M.
name: Tolba, T.
name: Tsang, R.
name: Vogel, P.
name: Vuilleumier, J. -L.
name: Wagenpfeil, M.
name: Waite, A.
name: Walton, J.
name: Walton, T.
name: Weber, M.
name: Wen, L. J.
name: Wichoski, U.
name: Yang, L.
name: Yen, Y. -R.
name: Zeldovich, O. Ya.
name: Zettlemoyer, J.
name: Ziegler, T.
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Physics - Experiment (hep-ex)
subject: Nuclear Experiment (nucl-ex)
subject: FOS: Physical sciences

description: Searches for double beta decay of $^{134}$Xe were performed with EXO-200, a single-phase liquid xenon detector designed to search for neutrinoless double beta decay of $^{136}$Xe. Using an exposure of $29.6\text{ kg}\!\cdot\!\text{yr}$, the lower limits of $\text{T}_{1/2}^{2νβ\!β}>8.7\cdot10^{20}\text{ yr}$ and $\text{T}_{1/2}^{0νβ\!β}>1.1\cdot10^{23}\text{ yr}$ at 90% confidence level were derived, with corresponding half-life sensitivities of $1.2\cdot10^{21}\text{ yr}$ and $1.9\cdot10^{23}\text{ yr}$. These limits exceed those in the literature for $^{134}$Xe, improving by factors of nearly $10^{5}$ and 2 for the two antineutrino and neutrinoless modes, respectively.
description: 8 pages, 4 figures
Tomonaga-Luttinger spin liquid in the spin-1/2 inequilateral diamond-chain compound K$_3$Cu$_3$AlO$_2$(SO$_4$)$_4$
Creators: name: Fujihala, M.
name: Koorikawa, H.
name: Mitsuda, S.
name: Morita, K.
name: Tohyama, T.
name: Tomiyasu, K.
name: Koda, A.
name: Okabe, H.
name: Itoh, S.
name: Yokoo, T.
name: Ibuka, S.
name: Tadokoro, M.
name: Itoh, M.
name: Sagayama, H.
name: Kumai, R.
name: Murakami, Y.
name: Nakamura, D.
Publisher: name: arXiv
Year: 2017
Subjects: subject: Strongly Correlated Electrons (cond-mat.str-el)
subject: FOS: Physical sciences

description: K$_3$Cu$_3$AlO$_2$(SO$_4$)$_4$ is a highly one-dimensional spin-1/2 inequilateral diamond-chain antiferromagnet. Spinon continuum and spin-singlet dimer excitations are observed in the inelastic neutron scattering spectra, which is in excellent agreement with a theoretical prediction: a dimer-monomer composite structure, where the dimer is caused by strong antiferromagnetic (AFM) coupling and the monomer forms an almost isolated quantum AFM chain controlling low-energy excitations. Moreover, muon spin rotation/relaxation spectroscopy shows no long-range ordering down to 90~mK, which is roughly three orders of magnitude lower than the exchange interaction of the quantum AFM chain. K$_3$Cu$_3$AlO$_2$(SO$_4$)$_4$ is, thus, regarded as a compound that exhibits a Tomonaga-Luttinger spin liquid behavior at low temperatures close to the ground state.
Fine structure of the diffraction cone: manifestation of t channel unitarity
Creators: name: Jenkovszky, László
name: Szanyi, István
Publisher: name: arXiv
Year: 2017
Subjects: subject: High Energy Physics - Phenomenology (hep-ph)
subject: High Energy Physics - Experiment (hep-ex)
subject: FOS: Physical sciences

description: We show that the deviation from exponential behavior of the diffraction cone observed near t=-0.1 GeV^2 both at ISR and the LHC (so-called break) follows from a two-pion loop in the t channel, imposed by unitarity. By using a simple Regge-pole model, we extrapolate the "break" from the ISR energy region to that of the LHC.
description: 11 pages, 13 figures; Invited talk at the 2016 Zim\'anyi Winter School, presented by I. Szanyi
Propagation and jamming dynamics in Heisenberg spin ladders
Creators: name: Krimphoff, Carlo B.
name: Haque, Masudul
name: Läuchli, Andreas M.
Publisher: name: arXiv
Year: 2016
Subjects: subject: Quantum Gases (cond-mat.quant-gas)
subject: FOS: Physical sciences

description: We investigate the propagation dynamics of initially localized excitations in spin-1/2 Heisenberg ladders. We consider initial states with two overturned spins, either on neighboring sites on the same leg or on the two sites of a single rung, in an otherwise polarized (ferromagnetic) background. Compared to the corresponding dynamics in a chain (single leg), we observe several additional modes of propagation. We connect these propagation modes to features of the spectrum of the ladder system, and to different effective models corresponding to different segments of the spectrum. In addition to the regular propagation modes, we observe for one mode a peculiar `jamming' dynamics where components of the excitations remain localized in an unusual manner. A comparison with the spin-1 bilinear-biquadratic chain is developed and explored, where a similar phenomenon is shown to occur.
description: 11+8 pages, 12+4 figures