Vorontsov-Velyaminov rows: Straight segments in the spiral arms of galaxies

Chernin, A. D.; Засов, А. В.; Архипова, В. П.; Kravtsova, A. S.

doi:10.1134/1.20393

Cited by 10 publications

(16 citation statements)

References 9 publications

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“…I assume that the local flattening of the front may have the same physical nature as the universal stability of a flat shock against any weak perturbations that disturb its front surfaces. [An assumption like this was earlier suggested in a study of straight outer segments observed in barred spirals (Chernin 1997). ] I do not try to develop a complete theory here; rather, I confine myself to a discussion based on the well‐known gas‐dynamical results concerning the stability of a flat shock.…”

Section: The Physics Of Rows: Gas Dynamics In Spiral Armssupporting

confidence: 62%

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Spiral patterns with straight arm segments

Chernin¹

1999

Monthly Notices of the Royal Astronomical Society

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The phenomenon of ‘rows’, which are straight geometrical segments in the spiral arms of galaxies, is studied. The Whirlpool nebula, Messier 51 (NGC 5194) in Canes Venatici, is considered to be an example of a giant grand design galaxy. Optical photographs, Hα, ultraviolet and far‐ultraviolet images, CO, 21‐cm and synchrotron emission maps, and a Ks‐band mosaic of M51 are studied. With this observational material, multiple rows can be recognized in the spiral arms of the galaxy. The rows comprise a major part of the arms. The lengths of the rows increase almost linearly with distance from the centre. They intersect one another at an (average) angle ≈2π/3. A possible physical explanation of the phenomenon of rows is discussed on the basis of the assumption that the formation of straight arm segments might be due to the gas‐dynamical effect of stability of flat shock fronts, and the tendency of a slightly curved shock front to become flat. A quantitative flattening criterion enables an explanation of the geometrical properties of the arm patterns found in M51 and also in M101. A brief list of spirals with rows is given.

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Section: The Physics Of Rows: Gas Dynamics In Spiral Armssupporting

confidence: 62%

“…Can disturbers and/or resonances explain the observed increase of the sizes of rows with distance from the centre? Can they also explain the existence of dust spiral arms turning into straight lines (see, for references, Chernin 1997) as the distance from the centre increases?…”

Section: Discussionmentioning

confidence: 99%

Spiral patterns with straight arm segments

Chernin¹

1999

Monthly Notices of the Royal Astronomical Society

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“…4). NGC 4303: This SBbc ( T = 4) galaxy has a small bar inside far extending spiral structure whose inner part shows straight arm segments, sometimes called ‘Vorontsov–Velyaminov rows’ (Chernin et al 2000). This structure is reproduced with a narrow pattern speed range (see Fig.…”

Section: Notes On Individual Galaxiesmentioning

confidence: 99%

Model-based pattern speed estimates for 38 barred galaxies

Rautiainen

Salo

Laurikainen

2008

Monthly Notices of the Royal Astronomical Society

102

146

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We have modelled 38 barred galaxies by using near-IR and optical data from the Ohio State University Bright Spiral Galaxy Survey. We constructed the gravitational potentials of the galaxies from $H$-band photometry, assuming constant mass-to-light ratio. The halo component we chose corresponds to the so called universal rotation curve. In each case, we used the response of gaseous and stellar particle disc to rigidly rotating potential to determine the pattern speed. We find that the pattern speed of the bar depends roughly on the morphological type. The average value of corotation resonance radius to bar radius, $\mathcal{R}$, increases from $1.15 \pm 0.25$ in types SB0/a -- SBab to $1.44 \pm 0.29$ in SBb and $1.82\pm 0.63$ in SBbc -- SBc. Within the error estimates for the pattern speed and bar radius, all galaxies of type SBab or earlier have a fast bar ($\mathcal{R} \le 1.4$), whereas the bars in later type galaxies include both fast and slow rotators. Of 16 later type galaxies with a nominal value of $\mathcal{R} > 1.4$, there are five cases, where the fast rotating bar is ruled out by the adopted error estimates. We also study the correlation between the parameter $\mathcal{R}$ and other galactic properties. The clearest correlation is with the bar size: the slowest bars are also the shortest bars when compared to the galaxy size. A weaker correlation is seen with bar strength in a sense that slow bars tend to be weaker. These correlations leave room for a possibility that the determined pattern speed in many galaxies corresponds actually that of the spiral, which rotates more slowly than the bar. No clear correlation is seen with either the galaxy luminosity or colour.Comment: 18 pages, 13 figures, accepted for publication in MNRA

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“…However, not all spiral arms are well described by logarithmic spirals, especially because the spiral arms in many galaxies branch, and often become open at the disc periphery. Moreover, as shown by Chernin et al (2000), many spiral arms have straight segments. As in our method, this technique implicitly assumes that the spirals are monotonic, but imposes stricter limitations on the form of spiral arms.…”

Section: Fitting Logarithmic or Other Forms Of Spirals To The Observementioning

confidence: 94%

Using an assumption about the monotony of spiral arms to determine the orientation angles of galaxies

Fridman¹,

Poltorak²

2010

Monthly Notices of the Royal Astronomical Society

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A method is proposed for the determination of the position and inclination angles of the plane of a spiral galaxy based on the assumption that every spiral arm is a monotonic function of the radius against azimuthal angle. This method may yield more accurate results than the more commonly employed isophote method, which is subject to a number of drawbacks. Analytical study, calibration against other methods and examples of application of the proposed method to real galaxies are presented.

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Vorontsov-Velyaminov rows: Straight segments in the spiral arms of galaxies

Cited by 10 publications

References 9 publications

Spiral patterns with straight arm segments

Spiral patterns with straight arm segments

Model-based pattern speed estimates for 38 barred galaxies

Using an assumption about the monotony of spiral arms to determine the orientation angles of galaxies

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