Chapter 10: The Sun-
... • AdLIGO estimate: Tens to >100 per year • Strong bias towards massive binaries Heavy things exchange • Low frequencies mean num rel is especially important f ...
... • AdLIGO estimate: Tens to >100 per year • Strong bias towards massive binaries Heavy things exchange • Low frequencies mean num rel is especially important f ...
Winds from clusters with non-uniform stellar distribution
... We present analytic and numerical models of the `cluster wind' resulting from the multiple interactions of the winds ejected by the stars of a dense cluster of massive stars. We consider the case in which the distribution of stars (i.e., the number of stars per unit volume) within the cluster is sph ...
... We present analytic and numerical models of the `cluster wind' resulting from the multiple interactions of the winds ejected by the stars of a dense cluster of massive stars. We consider the case in which the distribution of stars (i.e., the number of stars per unit volume) within the cluster is sph ...
Our galaxy is the centre of the universe, `quantized` red shifts show
... velocities’, as if they were caused by a Doppler shift. Unfortunately, that practice has confused the public, the media, and even undergraduate astronomy students into thinking of the redshifts as being caused mainly by velocities. Figure 4 shows more recent data on the redshift-distance relation ou ...
... velocities’, as if they were caused by a Doppler shift. Unfortunately, that practice has confused the public, the media, and even undergraduate astronomy students into thinking of the redshifts as being caused mainly by velocities. Figure 4 shows more recent data on the redshift-distance relation ou ...
Sunyaev±Zel'dovich distortion from early galactic winds Subhabrata Majumdar, Biman B. Nath
... We consider a large range of values for 3 # zin , 15: This assumption of a single epoch can be justified to some extent because of the fact that after the first objects of mass of order ,108 M( start shining and outflowing, the resulting UV background radiation and the winds both inhibit the further ...
... We consider a large range of values for 3 # zin , 15: This assumption of a single epoch can be justified to some extent because of the fact that after the first objects of mass of order ,108 M( start shining and outflowing, the resulting UV background radiation and the winds both inhibit the further ...
The Interstellar Medium in High Redshift Galaxies Comes of Age
... Studying the astrochemistry of the early Universe is crucial for understanding the properties of molecular gas in galaxy formation and for providing fundamental constraints on galaxy evolution. To date, a fairly small number of species, other than CO, have been detected at z > 2 (e.g. HCN, HNC, CN, ...
... Studying the astrochemistry of the early Universe is crucial for understanding the properties of molecular gas in galaxy formation and for providing fundamental constraints on galaxy evolution. To date, a fairly small number of species, other than CO, have been detected at z > 2 (e.g. HCN, HNC, CN, ...
Galaxy S-Stars Exhibit Orbital Angular Momentum Quantization per
... The innermost stars of our Galaxy, called S-stars, are in Keplerian orbits about a proposed [1] black hole of mass 4.3 ± 0.3 million solar masses. Their orbital planes appear to have random orientations, their orbital eccentricities range from 0.131 to 0.963 with no apparent pattern, and their origi ...
... The innermost stars of our Galaxy, called S-stars, are in Keplerian orbits about a proposed [1] black hole of mass 4.3 ± 0.3 million solar masses. Their orbital planes appear to have random orientations, their orbital eccentricities range from 0.131 to 0.963 with no apparent pattern, and their origi ...
Weak gravitational lensing
While the presence of any mass bends the path of light passing near it, this effect rarely produces the giant arcs and multiple images associated with strong gravitational lensing. Most lines of sight in the universe are thoroughly in the weak lensing regime, in which the deflection is impossible to detect in a single background source. However, even in these cases, the presence of the foreground mass can be detected, by way of a systematic alignment of background sources around the lensing mass. Weak gravitational lensing is thus an intrinsically statistical measurement, but it provides a way to measure the masses of astronomical objects without requiring assumptions about their composition or dynamical state.