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Query : 2014A&A...571A..95F |

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2014A&A...571A..95F -
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Astronomy and Astrophysics, volume 571A, 95-95 (2014/11-1)
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On the probability distribution function of the mass surface density of molecular clouds. II.
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FISCHERA J.
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Abstract (from CDS):
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The probability distribution function (PDF) of the mass surface density of molecular clouds provides essential information about the structure of molecular cloud gas and condensed structures out of which stars may form. In general, the PDF shows two basic components: a broad distribution around the maximum with resemblance to a log-normal function, and a tail at high mass surface densities attributed to turbulence and self-gravity. In a previous paper, the PDF of condensed structures has been analyzed and an analytical formula presented based on a truncated radial density profile, ρ(r)=ρ_{c}/(1+(r/r_{0})^{2})^{n/2} with central density ρ_{c} and inner radius r_{0}, widely used in astrophysics as a generalization of physical density profiles. In this paper, the results are applied to analyze the PDF of self-gravitating, isothermal, pressurized, spherical (Bonnor-Ebert spheres) and cylindrical condensed structures with emphasis on the dependence of the PDF on the external pressure p_{ext} and on the overpressure q^{–1}=p_{c}/p_{ext}, where p_{c} is the central pressure. Apart from individual clouds, we also consider ensembles of spheres or cylinders, where effects caused by a variation of pressure ratio, a distribution of condensed cores within a turbulent gas, and (in case of cylinders) a distribution of inclination angles on the mean PDF are analyzed. The probability distribution of pressure ratios q^{–1} is assumed to be given by P(q^{–1})∝q^{–k1}/(1+(q_{0}/q)^{γ})^{(k1+k2)/γ}, where k_{1}, γ, k_{2}, and q_{0} are fixed parameters. The PDF of individual spheres with overpressures below ∼100 is well represented by the PDF of a sphere with an analytical density profile with n=3. At higher pressure ratios, the PDF at mass surface densities Σ≪Σ(0), where Σ(0) is the central mass surface density, asymptotically approaches the PDF of a sphere with n=2. Consequently, the power-law asymptote at mass surface densities above the peak steepens from P_{sph}(Σ)∝Σ^{–2} to P_{sph}(Σ)∝Σ^{–3}. The corresponding asymptote of the PDF of cylinders for the large q^{–1} is approximately given by P_{cyl}(Σ)∝Σ^{–4/3}/SQRT(1-(Σ/Σ(0))^{2/3}). The distribution of overpressures q^{–1} produces a power-law asymptote at high mass surface densities given by <P_{sph}(Σ)>∝Σ^{–2k2–1} (spheres) or <P_{cyl}(Σ)>∝Σ^{–2k2} (cylinders).

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Abstract Copyright:
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∼

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Journal keyword(s):
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ISM: clouds - methods: statistical - ISM: structure - methods: analytical
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Simbad objects:
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14

Number of rows : 14 |

N | Identifier | Otype |
ICRS (J2000) RA |
ICRS (J2000) DEC |
Mag U | Mag B | Mag V | Mag R | Mag I | Sp type |
#ref
1850 - 2021 |
#notes |
---|---|---|---|---|---|---|---|---|---|---|---|---|

1 | NAME Perseus Cloud | SFR | 03 35.0 | +31 13 | ~ | 1154 | 0 | |||||

2 | NAME Taurus Complex | SFR | 04 41.0 | +25 52 | ~ | 3765 | 0 | |||||

3 | NAME Ori A | MoC | 05 38 | -07.1 | ~ | 2787 | 0 | |||||

4 | NAME Ori B | MoC | 05 41 43.0 | -01 54 44 | ~ | 1230 | 0 | |||||

5 | NAME Rosette Molecular Cloud | MoC | 06 34.7 | +04 02 | ~ | 239 | 0 | |||||

6 | NAME Musca | Cld | 12 23 | -71.3 | ~ | 170 | 0 | |||||

7 | NAME Coalsack Nebula | DNe | 12 31 19 | -63 44.6 | ~ | 247 | 0 | |||||

8 | NAME Lupus I | Cld | 15 43 02.1 | -34 09 06 | ~ | 245 | 0 | |||||

9 | NAME Lupus III | SFR | 16 09.6 | -39 03 | ~ | 290 | 0 | |||||

10 | NAME Lupus V | MoC | 16 21 | -37.5 | ~ | 57 | 0 | |||||

11 | NAME Ophiuchus Molecular Cloud | SFR | 16 28 06 | -24 32.5 | ~ | 3213 | 1 | |||||

12 | LDN 204 | DNe | 16 47 47.3 | -12 05 16 | ~ | 52 | 0 | |||||

13 | LDN 1228 | DNe | 20 57 13 | +77 35.8 | ~ | 122 | 0 | |||||

14 | IC 5146 | OpC | 21 53 24 | +47 16.0 | ~ | 409 | 2 |

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2021.09.21-12:47:11

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