A reinvestigation of gas response to an ovally deformed gravitational potential

Takuya Matsuda; Minoru Inoue; Keisuke Sawada; Eiji Shima; Ken Ichi Wakamatsu

doi:10.1093/mnras/229.2.295

A reinvestigation of gas response to an ovally deformed gravitational potential

Takuya Matsuda, Minoru Inoue, Keisuke Sawada, Eiji Shima, Ken Ichi Wakamatsu

Research output: Contribution to journal › Article › peer-review

27 Citations (Scopus)

Abstract

The response of gas to an ovally deformed gravitational potential or a weak bar of a disc galaxy is investigated by the implicit Osher upwind scheme with second-order of accuracy in space and a 180x180 polar grid. Flow patterns obtained are sensitive to the pattern speed and the degree of a distortion from the axisymmetric part of the gravitational potential. Tightly wound spiral patterns were obtained even with a non-axisymmetric perturbation whose amplitude was as low as 0.01. Not only trailing arms but also leading arms are obtained in the inner region of model galaxies. When the amplitude of the non-axisymmetric perturbation is 0.05, we obtained loosely wound spirals.

Original language	English
Pages (from-to)	295-314
Number of pages	20
Journal	Monthly Notices of the Royal Astronomical Society
Volume	229
Issue number	2
DOIs	https://doi.org/10.1093/mnras/229.2.295
Publication status	Published - 1987 Jan
Externally published	Yes

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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title = "A reinvestigation of gas response to an ovally deformed gravitational potential",

abstract = "The response of gas to an ovally deformed gravitational potential or a weak bar of a disc galaxy is investigated by the implicit Osher upwind scheme with second-order of accuracy in space and a 180x180 polar grid. Flow patterns obtained are sensitive to the pattern speed and the degree of a distortion from the axisymmetric part of the gravitational potential. Tightly wound spiral patterns were obtained even with a non-axisymmetric perturbation whose amplitude was as low as 0.01. Not only trailing arms but also leading arms are obtained in the inner region of model galaxies. When the amplitude of the non-axisymmetric perturbation is 0.05, we obtained loosely wound spirals.",

author = "Takuya Matsuda and Minoru Inoue and Keisuke Sawada and Eiji Shima and Wakamatsu, {Ken Ichi}",

note = "Funding Information: This research was supported by the Grant-in-Aid for Scientific Research (61540183) of the Ministry of Education and Culture in Japan. The computations were performed on the FUJITSU VP-200 at the Data Processing Center of Kyoto University. TM thanks Dr H. C. Spruit for his discussion. Publisher Copyright: {\textcopyright} Royal Astronomical Society",

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AU - Matsuda, Takuya

AU - Inoue, Minoru

AU - Sawada, Keisuke

AU - Shima, Eiji

AU - Wakamatsu, Ken Ichi

N1 - Funding Information: This research was supported by the Grant-in-Aid for Scientific Research (61540183) of the Ministry of Education and Culture in Japan. The computations were performed on the FUJITSU VP-200 at the Data Processing Center of Kyoto University. TM thanks Dr H. C. Spruit for his discussion. Publisher Copyright: © Royal Astronomical Society

PY - 1987/1

Y1 - 1987/1

N2 - The response of gas to an ovally deformed gravitational potential or a weak bar of a disc galaxy is investigated by the implicit Osher upwind scheme with second-order of accuracy in space and a 180x180 polar grid. Flow patterns obtained are sensitive to the pattern speed and the degree of a distortion from the axisymmetric part of the gravitational potential. Tightly wound spiral patterns were obtained even with a non-axisymmetric perturbation whose amplitude was as low as 0.01. Not only trailing arms but also leading arms are obtained in the inner region of model galaxies. When the amplitude of the non-axisymmetric perturbation is 0.05, we obtained loosely wound spirals.

AB - The response of gas to an ovally deformed gravitational potential or a weak bar of a disc galaxy is investigated by the implicit Osher upwind scheme with second-order of accuracy in space and a 180x180 polar grid. Flow patterns obtained are sensitive to the pattern speed and the degree of a distortion from the axisymmetric part of the gravitational potential. Tightly wound spiral patterns were obtained even with a non-axisymmetric perturbation whose amplitude was as low as 0.01. Not only trailing arms but also leading arms are obtained in the inner region of model galaxies. When the amplitude of the non-axisymmetric perturbation is 0.05, we obtained loosely wound spirals.

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A reinvestigation of gas response to an ovally deformed gravitational potential

Abstract

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