Results 21 to 30 of about 2,700 (75)

Bulge formation from SSCs in a responding cuspy dark matter halo [PDF]

, 2007
We simulate the bulge formation in very late-type dwarf galaxies from circumnuclear super star clusters (SSCs) moving in a responding cuspy dark matter halo (DMH). The simulations show that (1) the response of DMH to sinking of SSCs is detectable only in
Cora S. A., Huang J.-H., Jie‐Hao Huang, Liu W. H., Wen‐Hao Liu, Yan‐Ning Fu, Zu‐Gan Deng   +6 more
core   +3 more sources

Dark Energy From the Gravitational Wave Background With Scalar Field Dark Matter

Astronomische Nachrichten, Volume 346, Issue 3-4, March-May 2025.
ABSTRACT Recent observational results, such as those from pulsar timing arrays (PTA), suggest a low‐frequency Gravitational Wave Background (GWB) permeates our universe. This opens the possibility that gravitational waves could span a broader spectrum, potentially impacting cosmological scales.
Edwin L. Pérez‐Ochoa, Tonatiuh Matos
wiley   +1 more source

Self-consistent massive disks in triaxial dark matter halos [PDF]

, 2007
Galactic disks in triaxial dark matter halos become deformed by the elliptical potential in the plane of the disk in such a way as to counteract the halo ellipticity. We develop a technique to calculate the equilibrium configuration of such a disk in the
Alberto D. Bolatto, Brad K. Gibson, Chris Power, Gerhard O. E., Jeremy Bailin, Joshua D. Simon, Schoenmakers R. H. M.   +6 more
core   +2 more sources

Halpha rotation curves: the soft core question

, 2002
We present high resolution Halpha rotation curves of 4 late-type dwarf galaxies and 2 low surface brightness galaxies (LSB) for which accurate HI rotation curves are available from the literature.
Andrea Zacchei, Claudio Firmani, Conconi P., Danilo Marchesini, de Blok W. J. G., de Blok W. J. G., Elena D’Onghia, Emilio Molinari, Guido Chincarini, Navarro J. F., Paolo Conconi, Richter O.-G., Wechsler R. H.   +12 more
core   +1 more source

An extensive study of dynamical friction in dwarf galaxies: the role of stars, dark matter, halo profiles and MOND

, 2006
We investigate the in-spiraling timescales of globular clusters in dwarf spheroidal (dSph) and dwarf elliptical (dE) galaxies, due to dynamical friction. We address the problem of these timescales having been variously estimated in the literature as much
Begeman, Bekenstein, Binney, Binney, Binney, Blais-Ouellette, Bottema, Brada, Buonanno, Ciotti, Coleman, Colpi, De Blok, De Blok, Dubath, F. J. Sánchez-Salcedo, Fall, Fuchs, Gentile, Gentile, Goerdt, Gunn, Hashimoto, Hayashi, Held, Hernandez, Hernandez, Hodge, Hubble, Jin, Jorge Reyes-Iturbide, Just, Kazantzidis, King, Kleyna, Kleyna, Kleyna, Kregel, Lacey, Lake, Lotz, Mackey, Magorrian, Mateo, Mayer, McGaugh, Milgrom, Milgrom, Navarro, Navarro, Oh, Pointecouteau, Pryor, Read, Read, Sanders, Sanders, Spekkens, Stoehr, Sánchez-Salcedo, Sánchez-Salcedo, Sánchez-Salcedo, Taffoni, The, Tremaine, Van Den Bosch, Walcher, Walker, Walker, Wang, White, X. Hernandez, Łokas, Łokas, Łokas, Łokas   +75 more
core   +1 more source

Density Profiles of Cold Dark Matter Substructure: Implications for the Missing Satellites Problem

, 2004
The structural evolution of substructure in cold dark matter (CDM) models is investigated combining ``low-resolution'' satellites from cosmological N-body simulations of parent halos with N=10^7 particles with high-resolution individual subhalos orbiting
Ben Moore, Binney J., Chiara Mastropietro, Eke V. R., Fall S. M., Joachim Stadel, Jurg Diemand, Kauffmann G., Klypin A., Lucio Mayer, Stelios Kazantzidis   +10 more
core   +1 more source

Cuspy No More: How Outflows Affect the Central Dark Matter and Baryon Distribution in Lambda CDM Galaxies

, 2012
We examine the evolution of the inner dark matter (DM) and baryonic density profile of a new sample of simulated field galaxies using fully cosmological, Lambda CDM, high resolution SPH + N-Body simulations.
A. M. Brooks, A. Pontzen, A. Zolotov, Abdo, Adams, Agertz, Ahn, Avila Reese, Barnes, Bell, Belokurov, Benson, Bigiel, Bode, Bower, Boylan-Kolchin, Brook, Brooks, Brooks, Bruzual, Bullock, C. Christensen, Ceverino, Chemin, Choi, Christensen, Colín, Conroy, Croft, Dalal, Dalcanton, Dalcanton, Davé, de Blok, de Blok, de Souza, Dekel, Dekel, Dekel, Del Popolo, Donato, Eke, El-Zant, Elmegreen, Elson, Evans, F. Governato, Fall, Feldmann, Flores, Font, Geha, Geha, Gentile, Gnedin, Gnedin, Goerdt, Goerdt, Governato, Governato, Governato, Guedes, Haardt, Hopkins, J. Wadsley, Katz, Kazantzidis, Kennicutt, Kereš, Kirby, Knebe, Knollmann, Koda, Koposov, Krumholz, Kuzio de Naray, Lackner, Li, Loeb, Lovell, Macciò, Macciò, Macciò, Martin, Martinez, Mashchenko, Mashchenko, Mayer, Mayer, McGaugh, McQuinn, Mo, Moore, Moore, Moster, Navarro, Navarro, Navarro, Oh, Oh, Oh, Oppenheimer, Parry, Peñarrubia, Pontzen, Pontzen, Pontzen, Primack, Quinn, Rashkov, Read, Reed, Riess, Romano-Díaz, S. H. Oh, S. Shen, Saitoh, Shapley, Shen, Simon, Simon, Spergel, Spergel, Springel, Stadel, Stinson, Stoehr, Strigari, Strigari, Stringer, Swaters, Swaters, Sánchez-Janssen, T. Quinn, Tollerud, Tollerud, Tonini, van den Bosch, van der Wel, Viel, Vogelsberger, Wadsley, Walker, Walker, Walter, Willman, Zhang, Zolotov   +147 more
core   +1 more source

The real and apparent convergence of N-body simulations of the dark matter structures: is the Navarro-Frenk-White profile real?

, 2014
We consider the reasons why a cuspy NFW-like profile persistently occurs in N-body simulations, in contradiction to some astronomical observations. The routine method of testing the convergence of N-body simulations (in particular, the negligibility of ...
Baushev, Anton N.
core   +1 more source

Chandrasekhar's Dynamical Friction and non-extensive statistics

, 2016
The motion of a point like object of mass $M$ passing through the background potential of massive collisionless particles ($m
de Souza, R. E., Del Popolo, A., Delliou, Morgan Le, Lee, Xi-Guo, Lima, J. A. S., Silva, J. M.   +5 more
core   +1 more source

The structure of dark matter halos in hierarchical clustering theories [PDF]

, 1999
During hierarchical clustering, smaller masses generally collapse earlier than larger masses and so are denser on the average. The core of a small mass halo could be dense enough to resist disruption and survive undigested, when it is incorporated into a
Barrow J. D., Bartelmann M., Cole S. M., Lahav O., Narayan R., Navarro J. F., Padmanabhan T., Padmanabhan T., Sikvie P., Steinmetz M., Subramanian K., Subramanian K., Subramanian K., Tormen G.   +13 more
core   +3 more sources