Connexins and Atherosclerosis

Pfenniger, Anna; Roth, Isabelle; Kwak, Brenda R.

doi:10.1007/978-1-59745-489-6_23

Cited by 56 publications

(82 citation statements)

References 34 publications

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“…The bar is modelled as a Ferrers n = 2 potential, as laid out by Pfenniger (1984), and as such, is a triaxial ellipsoid. The equations for the bar are too complex to present here (for full details see Pfenniger 1984). The bar rotates as a rigid body.…”

Section: O D E L L I N G T H E D I S C a N D Ba Rmentioning

confidence: 99%

Probing the Galaxy's bars via the Hercules stream

Gardner

Flynn

2010

Monthly Notices of the Royal Astronomical Society

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It has been suggested that a resonance between a rotating bar and stars in the solar neighbourhood can produce the so called 'Hercules stream'. Recently, a second bar may have been identified in the Galactic centre, the so called 'long bar', which is longer and much flatter than the traditional Galactic bar, and has a similar mass. We looked at the dynamical effects of both bars, separately and together, on orbits of stars integrated backwards from local position and velocities, and a model of the Galactic potential which includes the bars directly. Both bars can produce Hercules like features, and allow us to measure the rotation rate of the bar(s). We measure a pattern speed, for both bars, of 1.87 +/- 0.02 times the local circular frequency. This is on par with previous measurements for the Galactic bar, although we do adopt a slightly different Solar motion. Finally, we identify a new kinematic feature in local velocity space, caused by the long bar, which is tempting to identify with the high velocity 'Arcturus' stream.Comment: 9 pages, 10 figures, Accepted to MNRAS, Corrected for errat

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Section: O D E L L I N G T H E D I S C a N D Ba Rmentioning

confidence: 99%

Probing the Galaxy's bars via the Hercules stream

Gardner

Flynn

2010

Monthly Notices of the Royal Astronomical Society

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“…Athanassoula et al 1983Athanassoula et al , 1990Teuben & Sanders 1985;Kaufmann & Patsis 2005;Contopoulos & Patsis 2006) or 3D models (e.g. Pfenniger 1984;Pfenniger & Friedli 1991;Patsis, Skokos & Athanassoula 2002a,b,c, 2003a. In most studies, an 'ad hoc' choice of model is made for the gravitational potential.…”

Section: Introductionmentioning

confidence: 99%

Orbital structure inN-body models of barred-spiral galaxies

Harsoula

Kalapotharakos

2009

Monthly Notices of the Royal Astronomical Society

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We study the orbital structure in a series of self‐consistent N‐body configurations simulating rotating barred galaxies with spiral and ring structures. We perform frequency analysis in order to measure the angular and the radial frequencies of the orbits at two different time snapshots during the evolution of each N‐body system. The analysis is done separately for the regular and the chaotic orbits. We thereby identify the various types of orbits, determine the shape and percentages of the orbits supporting the bar and the ring/spiral structures, and study how the latter quantities change during the secular evolution of each system. Although the frequency maps of the chaotic orbits are scattered, we can still identify concentrations around resonances. We give the distributions of frequencies of the most important populations of orbits. We explore the phase‐space structure of each system using projections of the 4D surfaces of section. These are obtained via the numerical integration not only of the orbits of test particles, but also of the real N‐body particles. We thus identify which domains of the phase space are preferred and which are avoided by the real particles. The chaotic orbits are found to play a major role in supporting the shape of the outer envelope of the bar as well as the rings and the spiral arms formed outside corotation.

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“…Vandervoort 1984). Pfenniger (1984) and Richstone & Tremaine (1984) included kinematic moments in this method, and Rix et al (1997) showed how to include observed LOSVDs. A number of groups have developed independent numerical implementations of Schwarzschild method for axisymmetric geometry which fit the projected surface brightness and LOSVDs of early-type galaxies in detail (van der Marel et al 1998;Gebhardt et al 2000;Thomas et al 2004;Valluri, Merritt & Emsellem 2004;Cappellari et al 2006).…”

Section: Introductionmentioning

confidence: 99%

Recovery of the internal orbital structure of galaxies

Ven¹,

Zeeuw²,

Bosch³

2008

Monthly Notices RAS

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We construct axisymmetric and triaxial galaxy models with a phase-space distribution function that depends on linear combinations of the three exact integrals of motion for a separable potential. These Abel models, first introduced by Dejonghe & Laurent and subsequently extended by Mathieu & Dejonghe, are the axisymmetric and triaxial generalisations of the well-known spherical Osipkov-Merritt models. We show that the density and higher order velocity moments, as well as the line-of-sight velocity distribution (LOSVD) of these models can be calculated efficiently and that they capture much of the rich internal dynamics of early-type galaxies. We build a triaxial and oblate axisymmetric galaxy model with projected kinematics that mimic the two-dimensional kinematic observations that are obtained with integral-field spectrographs such as SAURON. We fit the simulated observations with axisymmetric and triaxial dynamical models constructed with our numerical implementation of Schwarzschild's orbit-superposition method. We find that Schwarzschild's method is able to recover the internal dynamics and three-integral distribution function of realistic models of early-type galaxies.Comment: 34 pages, 21 figures; companion paper at arXiv:0712.0113; accepted for publication in MNRAS; PDF file with full resolution figures at http://www.sns.ias.edu/~glenn/vdven_abel.pd

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Connexins and Atherosclerosis

Cited by 56 publications

References 34 publications

Probing the Galaxy's bars via the Hercules stream

Probing the Galaxy's bars via the Hercules stream

Orbital structure inN-body models of barred-spiral galaxies

Recovery of the internal orbital structure of galaxies

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