Standard

Estimating the dark halo mass from the relative thickness of stellar disks. / Sotnikova, N. Ya; Rodionov, S. A.

In: Astronomy Letters, Vol. 32, No. 10, 01.10.2006, p. 649-660.

Research output: Contribution to journal › Article › peer-review

Harvard

Sotnikova, NY & Rodionov, SA 2006, 'Estimating the dark halo mass from the relative thickness of stellar disks', Astronomy Letters, vol. 32, no. 10, pp. 649-660. https://doi.org/10.1134/S106377370610001X

APA

Sotnikova, N. Y., & Rodionov, S. A. (2006). Estimating the dark halo mass from the relative thickness of stellar disks. Astronomy Letters, 32(10), 649-660. https://doi.org/10.1134/S106377370610001X

Vancouver

Sotnikova NY, Rodionov SA. Estimating the dark halo mass from the relative thickness of stellar disks. Astronomy Letters. 2006 Oct 1;32(10):649-660. https://doi.org/10.1134/S106377370610001X

Author

Sotnikova, N. Ya ; Rodionov, S. A. / Estimating the dark halo mass from the relative thickness of stellar disks. In: Astronomy Letters. 2006 ; Vol. 32, No. 10. pp. 649-660.

BibTeX

@article{92837ab840df4285882cd61eab05602d,
title = "Estimating the dark halo mass from the relative thickness of stellar disks",
abstract = "We analyze the relationship between the mass of a spherical component and the minimum possible thickness of stable stellar disks. This relationship for real galaxies allows the lower limit on the dark halo mass to be estimated (the thinner the stable stellar disk is, the more massive the dark halo must be). In our analysis, we use both theoretical relations and numerical N-body simulations of the dynamical evolution of thin disks in the presence of spherical components with different density profiles and different masses. We conclude that the theoretical relationship between the thickness of disk galaxies and the mass of their spherical components is a lower envelope for the model data points. We recommend using this theoretical relationship to estimate the lower limit for the dark halo mass in galaxies. The estimate obtained turns out to be weak. Even for the thinnest galaxies, the dark halo mass within four exponential disk scale lengths must be more than one stellar disk mass.",
keywords = "Dark halo, Numerical simulations, Structure and dynamics of galaxies",
author = "Sotnikova, {N. Ya} and Rodionov, {S. A.}",
year = "2006",
month = oct,
day = "1",
doi = "10.1134/S106377370610001X",
language = "English",
volume = "32",
pages = "649--660",
journal = "Astronomy Letters",
issn = "1063-7737",
publisher = "МАИК {"}Наука/Интерпериодика{"}",
number = "10",

}

RIS

TY - JOUR

T1 - Estimating the dark halo mass from the relative thickness of stellar disks

AU - Sotnikova, N. Ya

AU - Rodionov, S. A.

PY - 2006/10/1

Y1 - 2006/10/1

N2 - We analyze the relationship between the mass of a spherical component and the minimum possible thickness of stable stellar disks. This relationship for real galaxies allows the lower limit on the dark halo mass to be estimated (the thinner the stable stellar disk is, the more massive the dark halo must be). In our analysis, we use both theoretical relations and numerical N-body simulations of the dynamical evolution of thin disks in the presence of spherical components with different density profiles and different masses. We conclude that the theoretical relationship between the thickness of disk galaxies and the mass of their spherical components is a lower envelope for the model data points. We recommend using this theoretical relationship to estimate the lower limit for the dark halo mass in galaxies. The estimate obtained turns out to be weak. Even for the thinnest galaxies, the dark halo mass within four exponential disk scale lengths must be more than one stellar disk mass.

AB - We analyze the relationship between the mass of a spherical component and the minimum possible thickness of stable stellar disks. This relationship for real galaxies allows the lower limit on the dark halo mass to be estimated (the thinner the stable stellar disk is, the more massive the dark halo must be). In our analysis, we use both theoretical relations and numerical N-body simulations of the dynamical evolution of thin disks in the presence of spherical components with different density profiles and different masses. We conclude that the theoretical relationship between the thickness of disk galaxies and the mass of their spherical components is a lower envelope for the model data points. We recommend using this theoretical relationship to estimate the lower limit for the dark halo mass in galaxies. The estimate obtained turns out to be weak. Even for the thinnest galaxies, the dark halo mass within four exponential disk scale lengths must be more than one stellar disk mass.

KW - Dark halo

KW - Numerical simulations

KW - Structure and dynamics of galaxies

UR - http://www.scopus.com/inward/record.url?scp=33749358777&partnerID=8YFLogxK

U2 - 10.1134/S106377370610001X

DO - 10.1134/S106377370610001X

M3 - Article

AN - SCOPUS:33749358777

VL - 32

SP - 649

EP - 660

JO - Astronomy Letters

JF - Astronomy Letters

SN - 1063-7737

IS - 10

ER -

ID: 33283716