The influence of interactions and minor mergers 
 on the structure of galactic disks

Schwarzkopf, U.; Dettmar, R.‐J.

doi:10.1051/aas:2000340

Cited by 16 publications

(21 citation statements)

References 21 publications

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“…Schwarzkopf & Dettmar (2000a confirmed this trend on a larger sample, but essentially because of a larger absolute thickness of interacting disks. They also noted that tidally interacting galaxies are more frequently warped and that the thickening was more noticeable in the outer parts.…”

Section: Introductionmentioning

confidence: 54%

“…Secondary inclination indicators (asymmetry of the minor axis profiles, apparent shift of the nucleus location from the symmetry plane) are in the same range as in local samples of highly inclined spirals (e.g. de Grijs & van der Kruit 1996;Schwarzkopf & Dettmar 2000a). Also, comparison with results of realistic numerical models for inclined spirals (e.g.…”

Section: General Characteristics Of Edge-on Disksmentioning

confidence: 63%

“…The factor for the vertical thickening (≥1.5) is approximately the same as for z ≈ 0 interacting spiral galaxies (∼1.5-2: Reshetnikov & Combes 1997;Schwarzkopf & Dettmar 2000a). The dependence of h/h z values on the rest-frame central surface brightness is shown in Fig.…”

Section: H/h Z Ratiomentioning

confidence: 68%

“…These values are typical for normal spiral disks at z ≈ 0 (e.g. Reshetnikov & Combes 1997;Schwarzkopf & Dettmar 2000a). However, the direct comparison of local and distant samples must be carried out with caution due to very different selection effects.…”

Section: Vertical Scalementioning

confidence: 86%

“…3 in Kregel et al 2002) In Fig. 6c we compare the Schwarzkopf & Dettmar (2000a) sample of non-interacting galaxies (the data in the Johnson R or Thuan & Gunn r filters). The fitting model avoids the central dust lane in the line-of-sight integration.…”

Section: Vertical Scalementioning

confidence: 99%

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On the global structure of distant galactic disks

Решетников

Dettmar

Combes³

2003

A&A

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Abstract. Radial and vertical profiles are determined for a sample of 34 edge-on disk galaxies in the HDFs, selected for their apparent diameter larger than 1.3 and their unperturbed morphology. The thickness and flatness of their galactic disks are determined and discussed with regard to evolution with redshift. We find that sub-L * spiral galaxies with z ∼ 1 have a relative thickness or flatness (characterized by h z /h the scaleheight to scalelength ratio) globally similar to those in the local Universe. A slight trend is however apparent, with the h z /h flatness ratio larger by a factor of ∼1.5 in distant galaxies if compared to local samples. In absolute value, the disks are smaller than in present-day galaxies. About half of the z ∼ 1 spiral disks show a non-exponential surface brightness distribution.

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Section: Introductionmentioning

confidence: 54%

Section: General Characteristics Of Edge-on Disksmentioning

confidence: 63%

Section: H/h Z Ratiomentioning

confidence: 68%

Section: Vertical Scalementioning

confidence: 86%

Section: Vertical Scalementioning

confidence: 99%

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On the global structure of distant galactic disks

Решетников

Dettmar

Combes³

2003

A&A

Self Cite

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Bars, Spiral Structure, and Secular Evolution in Disk Galaxies

Elmegreen¹

Island Universes

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Simulations and observations of galactic bars suggest they do not commonly evolve into bulges, although it is possible that the earliest bars formed bulges long ago, when galaxies were smaller, denser, and had more gas. The most highly evolved of today's bars may become lenses over a Hubble time. Most galaxies in the early Universe are extremely clumpy, with ∼ 10 8 − 10 9 M⊙ blue clumps that resemble in color and magnitude the isolated field objects nearby. The presence of blue and irregular bars at high redshift suggests that some bars formed primarily in the gas phase accompanied by giant starbursts, rather than in pure stellar disks like most models. Secular and non-secular processes that cause galaxies to evolve are summarized.

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Orbital dynamics of three-dimensional bars — III. Boxy/peanut edge-on profiles

Patsis

Skokos

Athanassoula

2002

Monthly Notices of the Royal Astronomical Society

145

183

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We present families, and sets of families, of periodic orbits that provide building blocks for boxy and peanut (hereafter b/p) edge-on profiles. We find cases where the b/p profile is confined to the central parts of the model and cases where a major fraction of the bar participates in this morphology. A b/p feature can be built either by 3D families associated with 3D bifurcations of the x1 family, or, in some models, even by families related with the z-axis orbits and existing over large energy intervals. The 'X' feature observed inside the boxy bulges of several edgeon galaxies can be attributed to the peaks of successive x1v1 orbits, provided their stability allows it. However in general, the x1v1 family has to overcome the obstacle of a S → → S transition in order to support the structure of a b/p feature. Other families that can be the backbones of b/p features are x1v4 and z3.1s. The morphology and the size of the boxy or peanut-shaped structures we find in our models are determined by the presence and stability of the families that support b/p features. The present study favours the idea that the observed edge-on profiles are the imprints of families of periodic orbits that can be found in appropriately chosen Hamiltonian systems, describing the potential of the bar.

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The influence of interactions and minor mergers on the structure of galactic disks

Cited by 16 publications

References 21 publications

On the global structure of distant galactic disks

On the global structure of distant galactic disks

Bars, Spiral Structure, and Secular Evolution in Disk Galaxies

Orbital dynamics of three-dimensional bars — III. Boxy/peanut edge-on profiles

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