On the Spiral Structure of Disk Galaxies. III. Comparison with Observations

Lin, C. C.; Yuan, C.; Shu, Frank H.

doi:10.1086/149907

Cited by 418 publications

(308 citation statements)

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“…which is the obvious generalization of the work of Lin, Yuan & Shu (1969) to the case of vertical velocity DFs.…”

Section: Zero Order Moments Of the Perturbed Dfmentioning

confidence: 82%

“…The most popular self-consistent fully analytical treatment available in literature to study the spiral arms is based so far on the DWT proposed by Lin, Yuan & Shu (1969), Marochnik & Suchkov (1969b), Marochnik & Suchkov (1969a). In these works, a sinusoidal perturbation to the axisymmetric potential for a discoidal stellar distribution is considered.…”

Section: Linear Response Theory To a Spiral Perturbation Patternmentioning

confidence: 99%

“…|kR| ≫ 1, we get rapidly to the form for the perturbed DF on the plane as: We are ready now to proceed to compute the first order moments of this DF that we adopted in our kinematic model. The moment of order zero and one was already carried out in numerical form by the authors in Appendix A of Lin, Yuan & Shu (1969) to the first order, and the second order central moments were recently proposed by Roca-Fàbrega et al (2014) in a work focused on the vertex deviation and the bracketing of the resonances. Nevertheless, in the original work by Lin, Yuan & Shu (1969) and in the work Roca-Fàbrega et al (2014) the numerical integral was passed over in favour of a more compact analytical formalism, and the divergences due to the resonances were not considered.…”

Section: Linear Response Theory To a Spiral Perturbation Patternmentioning

confidence: 99%

“…The treatment of Lin, Yuan & Shu (1969) is referred as Density Wave theory (DWT) and we will review in what follows the literature that attempts to validate it from the observational point of view.…”

Section: Introductionmentioning

confidence: 99%

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Spiral arm kinematics for Milky Way stellar populations

Pasetto

Natale

Kawata

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a new theoretical population synthesis model (the Galaxy Model) to examine and deal with large amounts of data from surveys of the Milky Way and to decipher the present and past structure and history of our own Galaxy.We assume the Galaxy to consist of a superposition of many composite stellar populations belonging to the thin and thick disks, the stellar halo and the bulge, and to be surrounded by a single dark matter halo component. A global model for the Milky Way's gravitational potential is built up self-consistently with the density profiles from the Poisson equation. In turn, these density profiles are used to generate synthetic probability distribution functions (PDFs) for the distribution of stars in colour-magnitude diagrams (CMDs). Finally, the gravitational potential is used to constrain the stellar kinematics by means of the moment method on a (perturbed)-distribution function. Spiral arms perturb the axisymmetric disk distribution functions in the linear response framework of density-wave theory where we present an analytical formula of the so-called 'reduction factor' using Hypergeometric functions.Finally, we consider an analytical non-axisymmetric model of extinction and an algorithm based on the concept of probability distribution function to handle colour magnitude diagrams with a large number of stars. A genetic algorithm is presented to investigate both the photometric and kinematic parameter space.This galaxy model represents the natural framework to reconstruct the structure of the Milky Way from the heterogeneous data set of surveys such as Gaia-ESO, SEGUE, APOGEE2, RAVE and the Gaia mission.

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“…which is the obvious generalization of the work of Lin, Yuan & Shu (1969) to the case of vertical velocity DFs.…”

Section: Zero Order Moments Of the Perturbed Dfmentioning

confidence: 82%

Section: Linear Response Theory To a Spiral Perturbation Patternmentioning

confidence: 99%

Section: Linear Response Theory To a Spiral Perturbation Patternmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Spiral arm kinematics for Milky Way stellar populations

Pasetto

Natale

Kawata

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Lin et al, 1969) rotate with angular velocities varying between Ω ∼ 20−60 rad/Gyr, in the outer and inner galactic regions, respectively (Bissantz et al, 2003). The inner part of the spiral galactic structure is probably corotating with the stars up to a distance of ∼ 3.4 kpc, corresponding approximately to the inner extremity of the Norma arm.…”

Section: From Soriamentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

230

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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The Fine Structure of the Spiral‐arms

Schmidt-Kaler

House

1976

Astron Nachr

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'An explanation for filaments inclined to the galactic plane observed in the next-inner spiral-arm is sought in terms of self-consistent z-oscillations. These filaments or ,,shingles" are obaerved to be N 1 . 4 kpc long, 70 pc thick and inclined to the plane by N 1 2 ' . In a collisionless axi-symmetric stellar system we simplify the BOLTZMANN and POISSON equations by assuming a constant density normal to the galactic plane up to 121 w 200 pc and by assuming a constant radial component of the spatial coordinates. The condition for selfconsistency in thelinear approximation resul tsin shingles 1.3 kpc long, inclined to the plane by 1 7 ' . The length of the shingles is independent of the radial distance R from the centre and the inclination depends inversely on R as is observed.Die Spiralarme der MilchstraDe weisen eine ca. IZ' gegen die Ebene geneigte Filamentstruktur (Schindeln) von etwa 1.5 kpc LILnge und nur 70 pc Dicke auf. Zur E r k l h n g dieses Phgnomens werden Dichtewellen in I (senkrecht zur galaktischen Ebene) in einem' stoBfreien axialsymmetrischen Sternsystem: betrachtet. Wir vereinfachen BOLTZYANN-und PoxssoN-Gleichung durch die Annahme konstanter Dichte e(z) bis l a1 = zoo pc und konstanter Radialkomponente der Raumgeschwindigkeiten. In erster Nilherung ergibt sich eine selbstkonsistente LOsung bei 1 = 1.3 kpc (eowie 1 7 O Neigung). Die Unge der Schindeln ist unabhiingig von der Entfernung R vom Zentmm, die Neigung nimmt mit I/R ab.

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On the Spiral Structure of Disk Galaxies. III. Comparison with Observations

Cited by 418 publications

References 0 publications

Spiral arm kinematics for Milky Way stellar populations

Spiral arm kinematics for Milky Way stellar populations

High-mass X-ray binaries in the Milky Way

The Fine Structure of the Spiral‐arms

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