2024MNRAS.534.1043B


Query : 2024MNRAS.534.1043B

2024MNRAS.534.1043B - Mon. Not. R. Astron. Soc., 534, 1043-1059 (2024/October-3)

Gravity or turbulence? - VI. The physics behind the Kennicutt-Schmidt relation.

BALLESTEROS-PAREDES J., ZAMORA-AVILES M., ROMAN-ZUNIGA C., PALAU A., CERVANTES-SODI B., GUTIERREZ-DAVILA K., CAMACHO V., JIMENEZ-ANDRADE E. and GAZOL A.

Abstract (from CDS):

We explain the large variety of star formation laws in terms of one single, simple law that can be inferred from the definition of the star formation rate and basic algebra. The resulting equation, ${\rm SFR}= {\epsilon _\mathrm{ff}}\ M_\mathrm{collapse}/{\tau _{\rm ff}}$, although it has been presented elsewhere, is interpreted in terms of clouds undergoing collapse rather than being turbulence supported, an idea that different groups have pursued this century. Under such assumption, one can explain the constancy of ${\epsilon _\mathrm{ff}}$, the different intra-cloud correlations observed in Milky Way's molecular clouds, as well as the resolved and unresolved extragalactic relationships between SFR and a measurement of the mass in CO, HCN, and CO + HI. We also explain why the slope of the correlation changes when the orbital time ${\tau _{\rm orb}}$ is considered instead of the free-fall time, and why estimations of the free-fall time from extragalactic observations skew the correlation, providing a false sublinear correlation. We furthermore show that the apparent nearly linear correlation between the star formation rate and the dynamical equilibrium pressure in the mid-plane of the galaxies, $P_{\rm DE}$, is just a consequence of $P_{\rm DE}$ values being dominated by the variation of the column density of molecular gas. All in all, we argue that the star formation law is driven by the collapse of cold, dense gas, which happens to be primarily molecular in the present Universe, and that the role of stellar feedback is just to shut down the star formation process, not to shape the star formation law.

Abstract Copyright: © 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.

Journal keyword(s): stars: formation - ISM: clouds - ISM: kinematics and dynamics - galaxies: general - galaxies: star formation

Simbad objects: 10

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Number of rows : 10
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 RAFGL 490 Or* 03 27 38.7928952784 +58 47 00.025298088           ~ 359 0
2 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1553 0
3 NAME California Molecular Cloud MoC 04 10.0 +39 00           ~ 188 1
4 NAME Ori A MoC 05 38 -07.1           ~ 3187 0
5 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1498 0
6 NAME Orion Molecular Cloud MoC 05 56 -01.8           ~ 1227 1
7 NAME Mon R2 HII 06 07 47.58 -06 22 42.6           ~ 789 2
8 NAME Musca Cld 12 23 -71.3           ~ 258 0
9 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3969 1
10 NAME Cyg X Cld 20 30 04.7973633 +40 51 36.002197           ~ 962 1

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