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  • 1
    Electronic Resource
    Electronic Resource
    Charon's size and an upper limit on its atmosphere from a stellar occultation (2006)
    [s.l.] : Nature Publishing Group
    Nature 439 (2006), S. 52-54 
    Details
    ISSN: 1476-4687
    Source: Nature Archives 1869 - 2009
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Notes: [Auszug] Pluto and its satellite, Charon (discovered in 1978; ref. 1), appear to form a double planet, rather than a hierarchical planet/satellite couple. Charon is about half Pluto's size and about one-eighth its mass. The precise radii of Pluto and Charon have remained uncertain, ...
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1038/nature04351
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    Paper (German National Licenses)
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  • 2
    Electronic Resource
    Electronic Resource
    The Elusive Dust Torus of NGC 1068 Unveiled by Adaptive Optics Observations from 2.2 µm TO 4.8 µm (1997)
    Springer
    Astrophysics and space science 248 (1997), S. 237-244 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Near-infrared, adaptive optics observations of AGN achieve a spatial resolution comparable to that of the Hubble Space Telescope at visible and ultraviolet wavelengths. Using the ESO adaptive optics system, we have mapped the nuclear region of NGC 1068 in the near-infrared at 2.2, 3.5 and 4.8 µm. These data show the presence of strong near-infrared emission within the central 100 pc around the nucleus. At the K, L and M bands, the dominant emission peak is unresolved at resolutions of 35 pc (K), 15 pc (L) and 23 pc (M). We find that the emission peaks at 2.2, 3.5 and 4.8 µm are offset by 0.3±0.1" south of the HST optical continuum peak. The infrared peaks are coincident with the HST imaging polarimetry center thought to mark the hidden nucleus. We conclude that the infrared emission peaks are also directly related with the hidden nucleus and that they outline the dusty torus around the central engine, as expected from current AGN models. From our first estimate of the fluxes in L and M, we derive a dust temperature of 750 K for the unresolved component.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1000546032704
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  • 3
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    Nonmonotonic spin relaxation and decoherence in graphene quantum dots with spin-orbit interactions (2014)
    American Physical Society (APS)
    Details
    Publication Date: 2014-03-20
    Description: Author(s): Marco O. Hachiya, Guido Burkard, and J. Carlos Egues We investigate the spin relaxation and decoherence in a single-electron graphene quantum dot with Rashba and intrinsic spin-orbit interactions. We derive an effective spin-phonon Hamiltonian via the Schrieffer-Wolff transformation in order to calculate the spin relaxation time T1 and decoherence tim... [Phys. Rev. B 89, 115427] Published Wed Mar 19, 2014
    Keywords: Surface physics, nanoscale physics, low-dimensional systems
    Print ISSN: 1098-0121
    Electronic ISSN: 1095-3795
    Topics: Physics
    Published by American Physical Society (APS)
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  • 4
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    Ballistic spin resonance in multisubband quantum wires (2014)
    American Physical Society (APS)
    Details
    Publication Date: 2014-03-26
    Description: Author(s): Marco O. Hachiya, Gonzalo Usaj, and J. Carlos Egues Ballistic spin resonance was experimentally observed in a quasi-one-dimensional wire by Frolov et al. [Nature (London) 458 , 868 (2009)NATUAS10.1038/nature07873]. The spin resonance was generated by a combination of an external static magnetic field and the oscillating effective spin-orbit magnetic f... [Phys. Rev. B 89, 125310] Published Tue Mar 25, 2014
    Keywords: Semiconductors II: surfaces, interfaces, microstructures, and related topics
    Print ISSN: 1098-0121
    Electronic ISSN: 1095-3795
    Topics: Physics
    Published by American Physical Society (APS)
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  • 5
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    Maxwell perturbations on asymptotically anti–de Sitter spacetimes: Generic boundary conditions and a new branch of quasinormal modes (2015)
    American Physical Society (APS)
    Details
    Publication Date: 2015-12-03
    Description: Author(s): Mengjie Wang (王梦杰), Carlos Herdeiro, and Marco O. P. Sampaio Perturbations of asymptotically anti-de-Sitter (AdS) spacetimes are often considered by imposing field vanishing boundary conditions (BCs) at the AdS boundary. Such BCs, of Dirichlet-type, imply a vanishing energy flux at the boundary, but the converse is, generically, not true. Regarding AdS as a g… [Phys. Rev. D 92, 124006] Published Tue Dec 01, 2015
    Keywords: General Relativity and Gravitation
    Print ISSN: 0556-2821
    Electronic ISSN: 1089-4918
    Topics: Physics
    Published by American Physical Society (APS)
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  • 6
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    Correlation effects and orbital magnetism of Co clusters (2016)
    American Physical Society (APS)
    Details
    Publication Date: 2016-06-29
    Description: Author(s): L. Peters, I. Di Marco, O. Grånäs, E. Şaşıoğlu, A. Altun, S. Rossen, C. Friedrich, S. Blügel, M. I. Katsnelson, A. Kirilyuk, and O. Eriksson Recent experiments on isolated Co clusters have shown huge orbital magnetic moments in comparison with their bulk and surface counterparts. These clusters hence provide the unique possibility to study the evolution of the orbital magnetic moment with respect to the cluster size and how competing int… [Phys. Rev. B 93, 224428] Published Mon Jun 27, 2016
    Keywords: Magnetism
    Print ISSN: 1098-0121
    Electronic ISSN: 1095-3795
    Topics: Physics
    Published by American Physical Society (APS)
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  • 7
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    Considerations on the role of fall-back discs in the final stages of the common envelope binary interaction (2016)
    Oxford University Press
    Details
    Publication Date: 2016-07-01
    Description: The common envelope interaction is thought to be the gateway to all evolved compact binaries and mergers. Hydrodynamic simulations of the common envelope interaction between giant stars and their companions are restricted to the dynamical, fast, in-spiral phase. They find that the giant envelope is lifted during this phase, but remains mostly bound to the system. At the same time, the orbital separation is greatly reduced, but in most simulations it levels off at values larger than measured from observations. We conjectured that during the post-in-spiral phase the bound envelope gas will return to the system. Using hydrodynamic simulations, we generate initial conditions for our simulation that result in a fall-back disc with total mass and angular momentum in line with quantities from the simulations of Passy et al. We find that the simulated fall-back event reduces the orbital separation efficiently, but fails to unbind the gas before the separation levels off once again. We also find that more massive fall-back discs reduce the orbital separation more efficiently, but the efficiency of unbinding remains invariably very low. From these results we deduce that unless a further energy source contributes to unbinding the envelope (such as was recently tested by Nandez et al.), all common envelope interactions would result in mergers. On the other hand, additional energy sources are unlikely to help, on their own, to reduce the orbital separation. We conclude by discussing our dynamical fall-back event in the context of a thermally regulated post-common envelope phase.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 8
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    Hydrodynamic simulations of the interaction between giant stars and planets (2016)
    Oxford University Press
    Details
    Publication Date: 2016-03-11
    Description: We present the results of hydrodynamic simulations of the interaction between a 10 Jupiter mass planet and a red or asymptotic giant branch stars, both with a zero-age main sequence mass of 3.5 M . Dynamic in-spiral time-scales are of the order of few years and a few decades for the red and asymptotic giant branch stars, respectively. The planets will eventually be destroyed at a separation from the core of the giants smaller than the resolution of our simulations, either through evaporation or tidal disruption. As the planets in-spiral, the giant stars’ envelopes are somewhat puffed up. Based on relatively long time-scales and even considering the fact that further in-spiral should take place before the planets are destroyed, we predict that the merger would be difficult to observe, with only a relatively small, slow brightening. Very little mass is unbound in the process. These conclusions may change if the planet's orbit enhances the star's main pulsation modes. Based on the angular momentum transfer, we also suspect that this star–planet interaction may be unable to lead to large-scale outflows via the rotation-mediated dynamo effect of Nordhaus and Blackman. Detectable pollution from the destroyed planets would only result for the lightest, lowest metallicity stars. We furthermore find that in both simulations the planets move through the outer stellar envelopes at Mach-3 to Mach-5, reaching Mach-1 towards the end of the simulations. The gravitational drag force decreases and the in-spiral slows down at the sonic transition, as predicted analytically.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 9
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    The effect of tides on the population of PN from interacting binaries (2016)
    Oxford University Press
    Details
    Publication Date: 2016-09-16
    Description: We have used the tidal equations of Zahn to determine the maximum orbital distance at which companions are brought into Roche lobe contact with their giant primary, when the primary expands during the giant phases. This is a key step when determining the rates of interaction between giants and their companions. Our stellar structure calculations are presented as maximum radii reached during the red and asymptotic giant branch (RGB and AGB, respectively) stages of evolution for masses between 0.8 and 4.0 M ( Z = 0.001–0.04) and compared with other models to gauge the uncertainty on radii deriving from details of these calculations. We find overall tidal capture distances that are typically 1–4 times the maximum radial extent of the giant star, where companions are in the mass range from 1 M J to a mass slightly smaller than the mass of the primary. We find that only companions at initial orbital separations between ~320 and ~630 R will be typically captured into a Roche lobe-filling interaction or a common envelope on the AGB. Comparing these limits with the period distribution for binaries that will make planetary nebula (PN), we deduce that in the standard scenario where all ~1–8 M stars make a PN, at most 2.5 per cent of all PN should have a post-common envelope central star binary, at odds with the observational lower limit of 15–20 per cent. The observed overabundance of post-interaction central stars of PN cannot be easily explained considering the uncertainties. We examine a range of explanations for this discrepancy.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 10
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    Two-loop stability of a complex singlet extended standard model (2015)
    American Physical Society (APS)
    Details
    Publication Date: 2015-07-17
    Description: Author(s): Raul Costa, António P. Morais, Marco O. P. Sampaio, and Rui Santos Motivated by the dark matter and the baryon asymmetry problems, we analyze a complex singlet extension of the Standard Model with a Z 2 symmetry (which provides a dark matter candidate). After a detailed two-loop calculation of the renormalization group equations for the new scalar sector, we study t… [Phys. Rev. D 92, 025024] Published Thu Jul 16, 2015
    Keywords: Field Theory, Formal Particle Theory
    Print ISSN: 0556-2821
    Electronic ISSN: 1089-4918
    Topics: Physics
    Published by American Physical Society (APS)
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