C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST01:05:07

2013A&A...551A..38P - Astronomy and Astrophysics, volume 551A, 38-38 (2013/3-1)

Ortho-H2 and the age of prestellar cores.


Abstract (from CDS):

Prestellar cores form from the contraction of cold gas and dust material in dark clouds before they collapse to form protostars. Several concurrent theories exist to describe this contraction but they are currently difficult to distinguish. One major difference is the timescale involved in forming the prestellar cores: some theories advocate nearly free-fall speed via, e.g., rapid turbulence decay, while others can accommodate much longer periods to let the gas accumulate via, e.g., ambipolar diffusion. To tell the difference between these theories, measuring the age of prestellar cores could greatly help. However, no reliable clock currently exists. We present a simple chemical clock based on the regulation of the deuteration by the abundance of ortho-H2 that slowly decays away from the ortho-para statistical ratio of 3 down to or less than 0.001. We use a chemical network fully coupled to a hydrodynamical model that follows the contraction of a cloud, starting from uniform density, and reaches a density profile typical of a prestellar core. We compute the N2D+/N2H+ ratio along the density profile. The disappearance of ortho-H2 is tied to the duration of the contraction and the N2D+/N2H+ ratio increases in the wake of the ortho-H2 abundance decrease. By adjusting the time of contraction, we obtain different deuteration profiles that we can compare to the observations. Our model can test fast contractions (from 104 to 106cm–3 in ∼0.5My) and slow contractions (from 104 to 106cm–3 in ∼5My). We have tested the sensitivity of the models to various initial conditions. The slow-contraction deuteration profile is approximately insensitive to these variations, while the fast-contraction deuteration profile shows significant variations. We found that, in all cases, the deuteration profile remains clearly distinguishable whether it comes from the fast collapse or the slow collapse. We also study the para-D2H+/ortho-H2D+ ratio and find that its variation is not monotonic, so it does not discriminate between models. Applying this model to L183 (=L134N), we find that the N2D+/N2H+ ratio would be higher than unity for evolutionary timescales of a few megayears independently of other parameters, such as cosmic ray ionization rate or grain size (within reasonable ranges). A good fit to the observations is only obtained for fast contraction (≤0.7My from the beginning of the contraction and ≤4My from the birth of the molecular cloud based on the need to keep a high ortho-H2 abundance when the contraction starts - ortho-H2/para-H2≥0.2 - to match the observations). This chemical clock therefore rules out slow contraction in L183 and steady-state chemical models, since steady state is clearly not reached here. This clock should be applied to other cores to help distinguish slow and fast contraction theories over a large sample of cases.

Abstract Copyright:

Journal keyword(s): astrochemistry - evolution - ISM: clouds - ISM: molecules - ISM: individual objects: L183 - ISM: abundances

Simbad objects: 5

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Number of rows : 5

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 LDN 1506C DNe 04 18 50.0 +25 19 15           ~ 8 0
2 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3479 0
3 LDN 183 MoC 15 54 12.2 -02 49 42           ~ 682 1
4 LDN 57 DNe 17 22 38.2 -23 49 34           ~ 283 1
5 NAME Vela Field reg ~ ~           ~ 149 0

    Equat.    Gal    SGal    Ecl

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