Therotation curveof a galaxy with an equatorial plane (for example a spiral galaxy has its spiral arms lying roughly in such a plane) is the plot of tangential velocity against distance from the centre for a particle (star or similar) moving in the equatorial plane. In practice it is not...
The rotation curve derived for NGC 1961 indicates a total mass greater than 10/sup 12/ M/sub sun/. This large value is confirmed by the correspondingly lar... VC Rubin,WK Ford,MS Roberts - 《Astrophysical Journal》 被引量: 109发表: 1979年 Effects of spacetime anisotropy on the galaxy ro...
Outer rotation curve of the Galaxy with VERA. II. Annual parallax and proper motion of the star-forming region IRAS21379+5106 "Outer rotation curve of the Galaxy with VERA II: annual parallax and proper motion of the star-forming region IRAS21379+5106", 2015, PASJ, v67, a68... N ...
this led to a remarkably small gravitational coupling G variation (about or less than 10^{-12} of its value per light-year), while also capable of generating galaxy rotation curves about as good as the best phenomenological dark matter profiles (considering both the rotation curve shape and th...
The flattening of the rotation curve suggests that the total mass of the galaxy within some radiusris increasing always with increase inr. This can only be explained if there is a large amount of invisible gravitating mass in these galaxies which is not giving out electromagnetic radiation. ...
The 50-years discrepancyin Galaxy Rotation Curves is in actuality a mismatch between the observed rotational velocities in galaxies and our predictions regarding these velocities. It is customary to plot those velocities as a function of the distance from the galactic center, as can be seen in the...
But to convert the velocity to kinematic distance, one needs to adopt a rotation curve for our Galaxy. For three different samples of tracers, we test different analytical forms. We find that the power-law expression, θ(R)/θ0 = 1.022 (R/R0)0.0803 with R0, θ0 = 8.34 kpc, 240 km...
1. Spinning motion of a celestial body or a group of gravitationally bound bodies, such as a galaxy, about an axis, as distinct from orbital revolution. Almost all celestial bodies show some degree of rotation. Young stars arrive on the main sequence with a high rotation rate; this results...
(2.18) were chosen so that the velocity curve becomes flat. Our choice is µ = 1 50 1 kpc , (2.24) y=3. (2.25) We thus obtain the square of the rotation velocity as a function of the distance r from the center of galaxy by rg 2π v2(r) = σ0 4π r dr′ dθ′r′e...
But to convert the velocity to kinematic distance, one needs to adopt a rotation curve for our Galaxy. For three different samples of tracers, we test different analytical forms. We find that the power-law expression, θ(R)/θ0 = 1.022 (R/R0)0.0803 with R0, θ0 = 8.34 kpc, 240 km...