The interaction of the spiral density wave and the Sun's galactic orbit

1978 ◽  
Vol 57 (2) ◽  
pp. 511-515 ◽  
Author(s):  
K. A. Innanen ◽  
A. T. Patrick ◽  
W. W. Duley
Keyword(s):  
Density Wave ◽  
Spiral Density Wave ◽  
Galactic Orbit

scholarly journals The Evolution of Giant Molecular Clouds

1980 ◽  
Vol 87 ◽  
pp. 137-149 ◽  
Author(s):  
Colin Norman ◽  
Joseph Silk
Keyword(s):  
Spatial Distribution ◽  
Star Formation ◽  
Molecular Clouds ◽  
Supernova Remnants ◽  
Density Wave ◽  
Collective Effects ◽  
Giant Molecular Clouds ◽  
Spiral Density Wave ◽  
External Galaxies ◽  
Co Observations

We discuss the origin, lifetime, destruction, spatial distribution and relation to star formation of giant molecular clouds. A coagulation model including the effects of spiral density wave shocks is described. We explore implications for CO observations of external galaxies. The collective effects of OB star winds and supernova remnants in disrupting clouds are considered.

scholarly journals 2D-Galactic chemical evolution: the role of the spiral density wave

2019 ◽  
Vol 490 (1) ◽  
pp. 665-682 ◽  
Author(s):  
M Mollá ◽  
S Wekesa ◽  
O Cavichia ◽  
Á I Díaz ◽  
B K Gibson ◽  
...  
Keyword(s):  
Star Formation ◽  
Chemical Evolution ◽  
Formation Rate ◽  
Density Wave ◽  
Spiral Wave ◽  
Elemental Abundance ◽  
Abundance Pattern ◽  
Spiral Density Wave ◽  
Azimuthal Symmetry

ABSTRACT We present a 2D chemical evolution code applied to a Milky Way type Galaxy, incorporating the role of spiral arms in shaping azimuthal abundance variations, and confront the predicted behaviour with recent observations taken with integral field units. To the usual radial distribution of mass, we add the surface density of the spiral wave and study its effect on star formation and elemental abundances. We compute five different models: one with azimuthal symmetry which depends only on radius, while the other four are subjected to the effect of a spiral density wave. At early times, the imprint of the spiral density wave is carried by both the stellar and star formation surface densities; conversely, the elemental abundance pattern is less affected. At later epochs, however, differences among the models are diluted, becoming almost indistinguishable given current observational uncertainties. At the present time, the largest differences appear in the star formation rate and/or in the outer disc (R ≥ 18 kpc). The predicted azimuthal oxygen abundance patterns for t ≤ 2 Gyr are in reasonable agreement with recent observations obtained with VLT/MUSE for NGC 6754.

The nearby spiral density–wave structure of the Galaxy

2017 ◽  
Vol 468 (3) ◽  
pp. 3361-3367 ◽  
Author(s):  
Evgeny Griv ◽  
Ing-Guey Jiang ◽  
Li-Gang Hou
Keyword(s):  
Density Wave ◽  
Wave Structure ◽  
Spiral Density Wave ◽  
The Galaxy

scholarly journals Spiral density wave generation by vortices in Keplerian flows

2005 ◽  
Vol 437 (1) ◽  
pp. 9-22 ◽  
Author(s):  
G. Bodo ◽  
G. Chagelishvili ◽  
G. Murante ◽  
A. Tevzadze ◽  
P. Rossi ◽  
...  
Keyword(s):  
Density Wave ◽  
Wave Generation ◽  
Spiral Density Wave

scholarly journals 5.19. A high resolution CO map of the inner region of M51

1998 ◽  
Vol 184 ◽  
pp. 249-250
Author(s):  
S. Aalto ◽  
S. Hüttemeister ◽  
N. Scoville ◽  
P. Thaddeus
Keyword(s):  
High Resolution ◽  
Spiral Galaxy ◽  
Density Wave ◽  
Linear Size ◽  
Structural Studies ◽  
Spiral Density Wave ◽  
Systemic Velocity ◽  
Grand Design ◽  
Inner Region ◽  
Design Spiral

M51, the Whirlpool Galaxy, at a distance of ≈ 9,6 Mpc and a systemic velocity of 465 km s−1, is the closest “Grand Design” spiral galaxy. Its low inclination (20°) makes it an excellent target for structural studies, e.g. the formation of arms in response to a spiral density wave causing gas streaming motions. We have obtained a high resolution, sensitive map of the inner 2.5′ of M51 using the Caltech six-element OVRO array. The map consists of a 19-field mosaic, taken using three different telescope configurations. The resolution is 2.5″, (corresponding to 115 pc linear size) and 3.5” for the robustly and naturally weigthed maps, respectively.

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