Gravity or turbulence? - II. Evolving column density probability distribution functions in molecular clouds

It has been recently shown that molecular clouds do not exhibit a unique shape for the column density probability distribution function (N-PDF). Instead, clouds without star formation seem to possess a lognormal distribution, while clouds with active star formation develop a power-law tail at high c...

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Vydáno v:	Monthly notices of the Royal Astronomical Society Ročník 416; číslo 2; s. 1436 - 1442
Hlavní autoři:	Ballesteros-Paredes, Javier, Vázquez-Semadeni, Enrique, Gazol, Adriana, Hartmann, Lee W., Heitsch, Fabian, Colín, Pedro
Médium:	Journal Article
Jazyk:	angličtina
Vydáno:	Oxford, UK Blackwell Publishing Ltd 01.09.2011 Wiley-Blackwell Oxford University Press
Témata:	Astronomy Astrophysics Earth, ocean, space Exact sciences and technology ISM: clouds ISM: general ISM: kinematics and dynamics Numerical analysis Star & galaxy formation stars: formation turbulence stars: formation ISM: clouds ISM: general turbulence ISM: kinematics and dynamics Turbulence Gravitational contraction High density Molecular clouds Digital simulation Column density Log normal distribution Star formation Dynamics Kinematics Probability density function Density fluctuation Power law Gravity
ISSN:	0035-8711, 1365-2966
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Abstract	It has been recently shown that molecular clouds do not exhibit a unique shape for the column density probability distribution function (N-PDF). Instead, clouds without star formation seem to possess a lognormal distribution, while clouds with active star formation develop a power-law tail at high column densities. The lognormal behaviour of the N-PDF has been interpreted in terms of turbulent motions dominating the dynamics of the clouds, while the power-law behaviour occurs when the cloud is dominated by gravity. In the present contribution, we use thermally bi-stable numerical simulations of cloud formation and evolution to show that, indeed, these two regimes can be understood in terms of the formation and evolution of molecular clouds: a very narrow lognormal regime appears when the cloud is being assembled. However, as the global gravitational contraction occurs, the initial density fluctuations are enhanced, resulting, first, in a wider lognormal N-PDF, and later, in a power-law N-PDF. We thus suggest that the observed N-PDF of molecular clouds are a manifestation of their global gravitationally contracting state. We also show that, contrary to recent suggestions, the exact value of the power-law slope is not unique, as it depends on the projection in which the cloud is being observed.
AbstractList	ABSTRACT It has been recently shown that molecular clouds do not exhibit a unique shape for the column density probability distribution function (N-PDF). Instead, clouds without star formation seem to possess a lognormal distribution, while clouds with active star formation develop a power-law tail at high column densities. The lognormal behaviour of the N-PDF has been interpreted in terms of turbulent motions dominating the dynamics of the clouds, while the power-law behaviour occurs when the cloud is dominated by gravity. In the present contribution, we use thermally bi-stable numerical simulations of cloud formation and evolution to show that, indeed, these two regimes can be understood in terms of the formation and evolution of molecular clouds: a very narrow lognormal regime appears when the cloud is being assembled. However, as the global gravitational contraction occurs, the initial density fluctuations are enhanced, resulting, first, in a wider lognormal N-PDF, and later, in a power-law N-PDF. We thus suggest that the observed N-PDF of molecular clouds are a manifestation of their global gravitationally contracting state. We also show that, contrary to recent suggestions, the exact value of the power-law slope is not unique, as it depends on the projection in which the cloud is being observed. [PUBLICATION ABSTRACT] It has been recently shown that molecular clouds do not exhibit a unique shape for the column density probability distribution function (N-PDF). Instead, clouds without star formation seem to possess a lognormal distribution, while clouds with active star formation develop a power-law tail at high column densities. The lognormal behaviour of the N-PDF has been interpreted in terms of turbulent motions dominating the dynamics of the clouds, while the power-law behaviour occurs when the cloud is dominated by gravity. In the present contribution, we use thermally bi-stable numerical simulations of cloud formation and evolution to show that, indeed, these two regimes can be understood in terms of the formation and evolution of molecular clouds: a very narrow lognormal regime appears when the cloud is being assembled. However, as the global gravitational contraction occurs, the initial density fluctuations are enhanced, resulting, first, in a wider lognormal N-PDF, and later, in a power-law N-PDF. We thus suggest that the observed N-PDF of molecular clouds are a manifestation of their global gravitationally contracting state. We also show that, contrary to recent suggestions, the exact value of the power-law slope is not unique, as it depends on the projection in which the cloud is being observed. ABSTRACT It has been recently shown that molecular clouds do not exhibit a unique shape for the column density probability distribution function (N‐PDF). Instead, clouds without star formation seem to possess a lognormal distribution, while clouds with active star formation develop a power‐law tail at high column densities. The lognormal behaviour of the N‐PDF has been interpreted in terms of turbulent motions dominating the dynamics of the clouds, while the power‐law behaviour occurs when the cloud is dominated by gravity. In the present contribution, we use thermally bi‐stable numerical simulations of cloud formation and evolution to show that, indeed, these two regimes can be understood in terms of the formation and evolution of molecular clouds: a very narrow lognormal regime appears when the cloud is being assembled. However, as the global gravitational contraction occurs, the initial density fluctuations are enhanced, resulting, first, in a wider lognormal N‐PDF, and later, in a power‐law N‐PDF. We thus suggest that the observed N‐PDF of molecular clouds are a manifestation of their global gravitationally contracting state. We also show that, contrary to recent suggestions, the exact value of the power‐law slope is not unique, as it depends on the projection in which the cloud is being observed.
Author	Hartmann, Lee W. Gazol, Adriana Ballesteros-Paredes, Javier Vázquez-Semadeni, Enrique Colín, Pedro Heitsch, Fabian
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Keywords	stars: formation ISM: clouds ISM: general turbulence ISM: kinematics and dynamics Turbulence Gravitational contraction High density Molecular clouds Digital simulation Column density Log normal distribution Star formation Dynamics Kinematics Probability density function Density fluctuation Power law Gravity
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Snippet	It has been recently shown that molecular clouds do not exhibit a unique shape for the column density probability distribution function (N-PDF). Instead,... ABSTRACT It has been recently shown that molecular clouds do not exhibit a unique shape for the column density probability distribution function (N‐PDF).... ABSTRACT It has been recently shown that molecular clouds do not exhibit a unique shape for the column density probability distribution function (N-PDF)....
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SubjectTerms	Astronomy Astrophysics Earth, ocean, space Exact sciences and technology ISM: clouds ISM: general ISM: kinematics and dynamics Numerical analysis Star & galaxy formation stars: formation turbulence
Title	Gravity or turbulence? - II. Evolving column density probability distribution functions in molecular clouds
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