Search results for "Chandrasekhar limit"
showing 4 items of 4 documents
Gravitational Waves from the Merging of White Dwarfs
2003
Binary white dwarfs emit gravitational waves with frequencies of up to a few mHz. As a consequence of the loss of angular momentum both components gradually approach and the gravitational waves emitted by the system increase both in amplitude and frequency (it is said that they chirp). In fact, the chirp of the galactic white dwarf binary population is expected to be the dominant source of noise at low frequencies. A fraction of these binaries, those separated by a distance smaller than roughly three solar radii, will eventually merge in a time shorter than a Hubble time. It is expected that during the merging they will emit gravitational waves transporting extremely valuable information ab…
The non-Gaussian distribution of galaxies gravitational fields
2016
We perform a theoretical analysis of the observational dependence between angular momentum of the galaxy clusters and their mass (richness), based on the method introduced in our previous paper. For that we obtain the distribution function of astronomical objects (like galaxies and/or smooth halos of different kinds) gravitational fields due to their tidal interaction. Within the statistical method of Chandrasekhar we are able to show that the distribution function is determined by the form of interaction between objects and for multipole (tidal) interaction it is never Gaussian. Our calculation permits to demonstrate how the alignment of galaxies angular momenta depend on the cluster richn…
The distribution of galaxies gravitational field stemming from their tidal interaction
2015
We calculate the distribution function of astronomical objects (like galaxies and/or smooth halos of different kinds) gravitational fields due to their tidal in- teraction. For that we apply the statistical method of Chandrasekhar (1943), used there to calculate famous Holtzmark distribution. We show that in our approach the distribution function is never Gaussian, its form being dictated by the potential of interaction between objects. This calculation permits us to perform a theoretical analysis of the relation between angular momentum and mass (richness) of the galaxy clusters. To do so, we follow the idea of Catelan & Theuns (1996) and Heavens & Peacock (1988). The main differen…
Stellar structure models in modified theories of gravity: Lessons and challenges
2019
The understanding of stellar structure represents the crossroads of our theories of the nuclear force and the gravitational interaction under the most extreme conditions observably accessible. It provides a powerful probe of the strong field regime of General Relativity, and opens fruitful avenues for the exploration of new gravitational physics. The latter can be captured via modified theories of gravity, which modify the Einstein-Hilbert action of General Relativity and/or some of its principles. These theories typically change the stellar structure equations, thus having a large impact on the astrophysical properties of the corresponding stars and opening a new window to constrain these …