Query : 2018A&A...615A..58Y

2018A&A...615A..58Y - Astronomy and Astrophysics, volume 615A, 58-58 (2018/7-1)

Constraint on ion-neutral drift velocity in the Class 0 protostar B335 from ALMA observations.


Abstract (from CDS):

Aims. Ambipolar diffusion can cause a velocity drift between ions and neutrals. This is one of the non-ideal magnetohydrodynamics (MHD) effects proposed to enable the formation of large-scale Keplerian disks with sizes of tens of au. To observationally study ambipolar diffusion in collapsing protostellar envelopes, we compare here gas kinematics traced by ionized and neutral molecular lines and discuss the implication on ambipolar diffusion.
Methods. We analyzed the data of the H13CO+ (3-2) and C18O (2-1) emission in the Class 0 protostar B335 obtained with our ALMA observations. We constructed kinematical models to fit the velocity structures observed in the H13CO+ and C18O emission and to measure the infalling velocities of the ionized and neutral gas on a 100au scale in B335.
Results. A central compact (∼1''-2'') component that is elongated perpendicular to the outflow direction and exhibits a clear velocity gradient along the outflow direction is observed in both lines and most likely traces the infalling flattened envelope. With our kinematical models, the infalling velocities in the H13CO+ and C18O emission are both measured to be 0.85±0.2km/s at a radius of 100au, suggesting that the velocity drift between the ionized and neutral gas is at most 0.3km/s at a radius of 100au in B335.
Conclusions. The Hall parameter for H13CO+ is estimated to be ≫1 on a 100au scale in B335, so that H13CO+ is expected to be attached to the magnetic field. Our non-detection or upper limit of the velocity drift between the ionized and neutral gas could suggest that the magnetic field remains rather well coupled to the bulk neutral material on a 100au scale in this source, and that any significant field-matter decoupling, if present, likely occurs only on a smaller scale, leading to an accumulation of magnetic flux and thus efficient magnetic braking in the inner envelope. This result is consistent with the expectation from the MHD simulations with a typical ambipolar diffusivity and those without ambipolar diffusion. On the other hand, the high ambipolar drift velocity of 0.5-1.0km/s on a 100au scale predicted in the MHD simulations with an enhanced ambipolar diffusivity by removing small dust grains, where the minimum grain size is 0.1 µm, is not detected in our observations. However, because of our limited angular resolution, we cannot rule out a significant ambipolar drift only in the midplane of the infalling envelope. Future observations with higher angular resolutions (∼0.1'') are needed to examine this possibility and ambipolar diffusion on a smaller scale.

Abstract Copyright: © ESO 2018

Journal keyword(s): stars: formation - ISM: kinematics and dynamics - ISM: individual objects: B335 - ISM: magnetic fields

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 - 2021
1 ICRF J193510.4+203154 Bz? 19 35 10.47291 +20 31 54.1542           ~ 43 1
2 LDN 663 DNe 19 36 55 +07 34.4           ~ 573 0
3 IRAS 19345+0727 FIR 19 37 01.03 +07 34 10.9           ~ 66 0
4 QSO B2032+107 QSO 20 35 22.3341660153 +10 56 06.789797044   17.96 16.37 17.4   ~ 168 1
5 4C 06.69 QSO 21 48 05.4585565234 +06 57 38.605396596   16.85 16.47 15.06   ~ 611 1

    Equat.    Gal    SGal    Ecl

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