2022A&A...657A.106L


Query : 2022A&A...657A.106L

2022A&A...657A.106L - Astronomy and Astrophysics, volume 657A, 106-106 (2022/1-1)

Tracing the large-scale magnetic field morphology in protoplanetary disks using molecular line polarization.

LANKHAAR B., VLEMMINGS W. and BJERKELI P.

Abstract (from CDS):


Context. Magnetic fields are fundamental to the accretion dynamics of protoplanetary disks and they likely affect planet formation. Typical methods to study the magnetic field morphology observe the polarization of dust or spectral lines. However, it has recently become clear that dust-polarization in ALMA's (Atacama Large (sub)Millimeter Array) spectral regime does not always faithfully trace the magnetic field structure of protoplanetary disks, which leaves spectral line polarization as a promising method for mapping the magnetic field morphologies of such sources.
Aims. We aim to model the emergent polarization of different molecular lines in the ALMA wavelength regime that are excited in protoplanetary disks. We explore a variety of disk models and molecules to identify those properties that are conducive to the emergence of polarization in spectral lines and may therefore be viably used for magnetic field measurements in protoplanetary disks.
Methods. We used POlarized Radiative Transfer Adapted to Lines in conjunction with the Line Emission Modeling Engine. Together, they allowed us to treat the polarized line radiative transfer of complex three-dimensional physical and magnetic field structures.
Results. We present simulations of the emergence of spectral line polarization of different molecules and molecular transitions in the ALMA wavelength regime. We find that molecules that thermalize at high densities, such as HCN, are also the most susceptible to polarization. We find that such molecules are expected to be significantly polarized in protoplanetary disks, while molecules that thermalize at low densities, such as CO, are only significantly polarized in the outer disk regions. We present the simulated polarization maps at a range of inclinations and magnetic field morphologies, and we comment on the observational feasibility of ALMA linear polarization observations of protoplanetary disks.
Conclusions. We conclude that those molecules with strong dipole moments and relatively low collision rates are most useful for magnetic field observations through line polarization measurements in high density regions such as protoplanetary disks.

Abstract Copyright: © ESO 2022

Journal keyword(s): magnetic fields - radiative transfer - polarization - stars: pre-main sequence - accretion, accretion disks

Simbad objects: 5

goto Full paper

goto View the references in ADS

Number of rows : 5
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 V* FU Ori Or* 05 45 22.3647842544 +09 04 12.291320064   10.72 9.60     F0Iab 774 1
2 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1787 1
3 THA 15-12 Or* 15 56 09.2066646912 -37 56 06.126118692   13.12 11.93 11.45   M0e 360 0
4 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 582 1
5 EM* AS 209 TT* 16 49 15.3034917000 -14 22 08.643317664   12.62 11.28     K4Ve 329 0

To bookmark this query, right click on this link: simbad:objects in 2022A&A...657A.106L and select 'bookmark this link' or equivalent in the popup menu


2023.01.30-21:20:26

© Université de Strasbourg/CNRS

    • Contact