In memory of Rem Viktorovich Khokhlov (1926-1977)

Kravtsov, Nikolai V; Polkovnikov, Boris F

doi:10.1070/qe1996v026n12abeh000885

Cited by 205 publications

(236 citation statements)

References 0 publications

Supporting

Mentioning

235

Contrasting

Order By: Relevance

“…The lower concentrations suggested by the M33 halo might indicate a low-density universe with a non-zero cosmological constant. A detailed discussion on the cosmological implications of our results requires, however, a more settled view of the mass±concentration dependence on cosmological models and on environmental effects (Kravtsov, Klypin & Khokhlov 1997;Navarro 1998;Avila-Rees et al 1999).…”

Section: Testing the Universal Density Profile In Hierarchical Clustementioning

confidence: 90%

“…Recent calculations of cosmological structure formation in hierarchical clustering CDM models (e.g. Navarro, Frenk & White 1996Kravtsov, Klypin & Khokhlov 1997) do not predict isothermal density distributions but haloes with a universal density profile which declines as R 21 for R , R s and as R 23 further out. R s is a scale radius which in terms of the virial radius R 200 and of the`concentration' parameter C can be written as R s R 200 aC.…”

Section: Testing the Universal Density Profile In Hierarchical Clustementioning

confidence: 99%

See 1 more Smart Citation

The extended rotation curve and the dark matter halo of M33

Corbelli

Salucci

2000

Monthly Notices of the Royal Astronomical Society

372

345

View full text Add to dashboard Cite

We present the 21‐cm rotation curve of the nearby galaxy M33 out to a galactocentric distance of 16 kpc (13 disc scalelengths). The rotation curve keeps rising out to the last measured point and implies a dark halo mass ≳5×1010 M⊙. The stellar and gaseous discs provide virtually equal contributions to the galaxy gravitational potential at large galactocentric radii, but no obvious correlation is found between the radial distribution of dark matter and the distribution of stars or gas. Results of the best fit to the mass distribution in M33 picture a dark halo which controls the gravitational potential from 3 kpc outward, with a matter density which decreases radially as R−1.3. The density profile is consistent with the theoretical predictions for structure formation in hierarchical clustering cold dark matter (CDM) models, and favours lower mass concentrations than those expected in the standard cosmogony.

show abstract

Section: Testing the Universal Density Profile In Hierarchical Clustementioning

confidence: 90%

Section: Testing the Universal Density Profile In Hierarchical Clustementioning

confidence: 99%

The extended rotation curve and the dark matter halo of M33

Corbelli

Salucci

2000

Monthly Notices of the Royal Astronomical Society

372

345

View full text Add to dashboard Cite

show abstract

“…For the interested reader, C1-8 have been generated with the adaptive mesh refinement code MLAPM (Knebe, Green & Binney 2001) and their properties have been discussed in detail in Warnick & Knebe (2006) and Warnick, Knebe & Power (2008). MW1 corresponds to model 'Box20' of Prada et al (2006) that has been simulated with the ART code (Kravtsov, Klypin & Khokhlov 1997). All other haloes (i.e.…”

Section: The Host Haloesmentioning

confidence: 99%

On the relation between the radial alignment of dark matter subhaloes and host mass in cosmological simulations

Knebe

Draganova

Power

et al. 2008

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

We explore the dependence of the radial alignment of subhaloes on the mass of the host halo they orbit in. As the effect is seen on a broad range of scales including massive clusters as well as galactic systems it only appears natural to explore this phenomenon by means of cosmological simulations covering the same range in masses. We have 25 well resolved host dark matter haloes at our disposal ranging from 1015 h−1 M⊙ down to 1012 h−1 M⊙ each consisting of order of a couple of million particles within the virial radius. We observe that subhaloes tend to be more spherical than isolated objects. Both the distributions of sphericity and triaxiality of subhaloes are Gaussian‐distributed with peak values of 〈s〉≈ 0.80 and 〈T〉≈ 0.56, irrespective of host mass. Interestingly, we note that the radial alignment is independent of host halo mass and the distribution of cos θ (i.e. the angle between the major‐axis Ea of each subhalo and the radius vector of the subhalo in the reference frame of the host) is well fitted by a simple power law P(cos θ) ∝ cos4θ with the same fitting parameters for all host haloes.

show abstract

“…Utilizing a parallel version of an established N-body code (Yahagi & Yoshii 2001;Yahagi 2005), the algorithm uses an adaptive mesh refinement technique to maintain accuracy (cf. Kravtsov, Klypin & Khokhlov 1997;Knebe, Green & Binney 2001;Yahagi & Yoshii 2001;Teyssier 2002). The simulation considered a region of the universe with a boxsize of 70 h −1 Mpc (commoving), with 512 3 particles, resulting in a particle mass of 3.04 × 10 8 h −1 M .…”

Section: Simulationsmentioning

confidence: 99%

The radial alignment of dark matter subhaloes: from simulations to observations

Knebe

Yahagi

Kase

et al. 2008

Monthly Notices of the Royal Astronomical Society: Letters

View full text Add to dashboard Cite

We explore the radial alignment of subhaloes in two‐dimensional projections of cosmological simulations. While most other recent studies focused on quantifying the signal utilizing the full three‐dimensional spatial information any comparison to observational data has to be done in projection along random lines‐of‐sight. We have a suite of well‐resolved host dark matter haloes at our disposal ranging from 6 × 1014 to 6 × 1013 h−1 M⊙. For these host systems, we do observe that the major axis of the projected two‐dimensional mass distribution of subhaloes aligns with its (projected) distance vector to the host's centre. The signal is actually stronger than the observed alignment. However, when considering only the innermost 10–20 per cent of the subhalo's particles for the two‐dimensional shape measurement, we recover the observed correlation. We further acknowledge that this signal is independent of subhalo mass.

show abstract

In memory of Rem Viktorovich Khokhlov (1926-1977)

Cited by 205 publications

References 0 publications

The extended rotation curve and the dark matter halo of M33

The extended rotation curve and the dark matter halo of M33

On the relation between the radial alignment of dark matter subhaloes and host mass in cosmological simulations

The radial alignment of dark matter subhaloes: from simulations to observations

Contact Info

Product

Resources

About