Dark energy domination in the Virgocentric flow

Chernin, A. D.; Караченцев, И. Д.; Nasonova, O. G.; Teerikorpi, P.; Valtonen, M. J.; Dolgachev, V. P.; Domozhilova, L. M.; Byrd, G. G.

doi:10.1051/0004-6361/201014912

Cited by 32 publications

(25 citation statements)

References 49 publications

(86 reference statements)

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“…We have previously (Chernin et al 2007a) discussed the data for the dwarf galaxies around the Local Group. The distance data come mainly from high accuracy observations of the TRGB (Tip of the Red Giant Branch) using the Hubble Space Telescope as reported by Karachentsev and his team in a series of papers (references e.g.…”

Section: The Hubble Diagram For the Group Environmentsmentioning

confidence: 99%

Dark energy in the environments of the Local Group, the M 81 group, and the CenA group: the normalized Hubble diagram

Teerikorpi¹,

Chernin

Караченцев

et al. 2008

A&A

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Context. Type Ia supernova observations on scales of thousands of Mpc show that the global expansion of the universe is accelerated by antigravity produced by the enigmatic dark energy contributing 3/4 of the total energy of the universe. Aims. Does antigravity act on small scales as well as large? As a continuation of our efforts to answer this crucial question we combine high accuracy observations of the galaxy flows around the Local Group and the nearby M 81 and CenA groups to observe the effect of the dark energy density on local scales of a few Mpc. Methods. We use an analytical model to describe non-uniform static space-time regions around galaxy groups. In this context it is useful to present the Hubble flow in a normalized Hubble diagram V/H v R v vs. r/R v , where the vacuum Hubble constant H v depends only on the cosmological vacuum density and the zero-gravity distance R v depends on the vacuum density and on the mass of the galaxy group. We have prepared the normalized Hubble diagrams for the LG, M 81 and CenA group environments for different values of the assumed vacuum energy density, using a total of about 150 galaxies, for almost all of which the distances have been measured by the HST. Results. The normalized Hubble diagram, where we identify dynamically different regions, is in agreement with the standard vacuum density (Ω v = 0.77 h −2 70 ), the out-flow of galaxies clearly being controlled by the minimum energy condition imposed by the central mass plus the vacuum density. A high vacuum density 1.6 h −2 70 violates the minimum energy limit, while a low density 0.1 h −2 70 leaves the start of the Hubble flow around 1−2 Mpc with the slope close to the global value obscure. We also consider the subtle relation of the zero-gravity radius R v to the zero-velocity distance R 0 appearing in the usual retarded expansion around a mass M: in a vacuumdominated flat universe R 0 ≈ 0.76 R v . Conclusions. The normalized Hubble diagram appears to be a good way to present and analyze physically different regions around mass clumps embedded in cosmological vacuum. The most natural interpretation of the diagram is that the local density of the dark energy is approximately equal to the density known from studies on global scales.

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Section: The Hubble Diagram For the Group Environmentsmentioning

confidence: 99%

Dark energy in the environments of the Local Group, the M 81 group, and the CenA group: the normalized Hubble diagram

Teerikorpi¹,

Chernin

Караченцев

et al. 2008

A&A

Self Cite

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“…, it is nevertheless receding at 1004 ± 70 km·s −1 [97]. Only galaxies within 9 ~ 11 Mpc have any realistic chance of eventually merging with it.…”

Section: Discussionmentioning

confidence: 97%

Planetary Heating by Neutrinos: Long-Term Habitats for Aquatic Life if Dark Energy Decays Favourably

Spivey¹

2013

JMP

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The potential cosmological and astrobiological implications of neutrinos are considered. Dark energy drives the current phase of accelerating cosmic expansion. Like inflation, it may decay in time to matter and radiation. However, since its energy density is minuscule in comparison, decay would be unlikely to inject such a rich variety of particles into the universe, and may instead be limited to the lowest energy fermions. Nonrelativistic neutrinos have the capacity to form stable, galaxy-engulfing haloes supported by degeneracy pressure, much like white dwarves and neutron stars. Conversely, bodies of mass 100M   can indefinitely rely on Coulomb forces for weight support. Opportunities for the mutual annihilation of electron neutrinos are largely confined to planets containing iron in the hcp phase. If dark energy decays primarily to neutrinos in 40 ~ 100 Gyr, then oceanic planets orbiting within the resulting haloes could provide long-term habitats for aquatic life with only lax constraints on the neutrino mass, 6 1 4 0m m  e V   . Various considerations now favour the possibility that neutrinos are Majorana particles with an inverted mass hierarchy and an electron neutrino mass in the vicinity of 50 meV. Sterile neutrinos of eV-mass may already be a significant component of dark matter, and could enhance planetary heating when active neutrino haloes become heavily depleted. An intriguing mechanism capable of regulating oceanic heat flux over a wide range of planetary masses is also described.

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“…Equation (109) was the argument given by Chernin et al (2010) to solve the Hubble-Sandage paradox on the scale of ∼10 Mpc (Sandage 1986(Sandage , 1999 observed that the local expansion was similar to that due to the Hubble flow. In the case of a shell i, its proper velocity at t t Fig.…”

Section: Discussionmentioning

confidence: 99%

Effects of the cosmological constant on cold dark matter clusters

Membrado

Pacheco

2014

A&A

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Context. Cold dark matter inhomogeneities are considered in a homogeneous background of matter, radiation, and the cosmological constant in a flat universe. Aims. We investigate the influence of the cosmological constant on the non-linear collapse of cold dark matter clusters. Methods. For simplicity, a spherical infall model has been used to describe the collapse of non-relativistic mass shells; besides, an average distribution of density around a cluster of galaxies has been taken. We have found that there is a limit to the mass of the average cluster, which is able to virialize; its value is {M VIR } MAX = 8.1 × 10 14 M . As expected, we found that shells present null proper acceleration at redshift values that are smaller than 0.755. Conclusions. We have noticed that the cosmological constant imposes an upper limit for the mass enclosed by shells, which are able to reach zero proper velocity. Hence, this mass is the maximum mass of the virialized core, {M VIR } MAX . For the average cluster addressed in this work, the value is 2.34 times the mass of the virialized core at present. Shells enclosing masses M > {M VIR } MAX achieve zero proper acceleration and speed up, moving away from the virialized core, and never reach a turn-around point. Shells with M {M VIR } MAX show zero proper aceleration at redshifts close to that at which the universe background acceleration is null. Finally, we have found that the relation between shell proper velocities and their radii can be adjusted by a straight line at z = 0 and from approximately 20 up to 40 Mpc; however, this line does not intercept the origin as velocities due to the Hubble flux do.

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Dark energy domination in the Virgocentric flow

Cited by 32 publications

References 49 publications

Dark energy in the environments of the Local Group, the M 81 group, and the CenA group: the normalized Hubble diagram

Dark energy in the environments of the Local Group, the M 81 group, and the CenA group: the normalized Hubble diagram

Planetary Heating by Neutrinos: Long-Term Habitats for Aquatic Life if Dark Energy Decays Favourably

Effects of the cosmological constant on cold dark matter clusters

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