<i>Planck</i>intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

Ade, Peter A. R.; Aghanim, N.; Alina, D.; Alves, M. I. R.; Aniano, G.; Armitage-Caplan, C.; Arnaud, M.; Arzoumanian, D.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bracco, A.; Burigana, C.; Cardoso, J.-F.; Catalano, A.; Chamballu, A.; Chiang, H. C.; Christensen, P. R.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; Bernardis, P. de; Rosa, A. de; Zotti, G. de; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, É.; Fanciullo, Lapo; Ferrière, K.; Finelli⋆, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Ghosh, T.; Giard, M.; Giraud‐Héraud, Y.; González‐Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.; Guillet, V.; Hansen, F. K.; Harrison, D. L.; Hélou, G.; Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneißl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J.-M.; Lasenby, A.; Lawrence, C. R.; Leonardi, R.; Levrier, F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López‐Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martín, P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, John A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Noviello, F.; Novikov, D.; Новиков, И. Д.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Pelkonen, Veli-Matti; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, É.; Polenta, G.; Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J.‐L.; Rachen, J. P.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rusholme, B.; Sandri, M.; Scott, D.; Soler, J. D.; Spencer, L. D.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Umana, G.; Valenziano, L.; Väliviita, J.; Tent, B. Van; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Zonca, A.

doi:10.1051/0004-6361/201424086

Cited by 124 publications

(14 citation statements)

References 50 publications

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“…As an example, previous studies have found an inverse correlation between the polarization fractionP and the local dispersion of magnetic field orientations at several scales in molecular clouds (Planck Collaboration et al 2015a, 2015bFissel et al 2016;Koch et al 2018). Such a measure toward B1-c would support the hypothesis of a complex but unresolved polarization structure, and higher-resolution observations using interferometric facilities would provide further evidence to confirm or disprove this scenario.…”

Section: Polarization Fraction and Grain Alignmentmentioning

confidence: 72%

The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-forming Region

Coudé¹,

Bastien²,

Houde³

et al. 2019

ApJ

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We present the POL-2 850 μm linear polarization map of the Barnard1 clump in the Perseus molecular cloud complex from the B-fields In STar-forming Region Observations survey at the James Clerk Maxwell Telescope. We find a trend of decreasing polarization fraction as a function of total intensity, which we link to depolarization effects toward higher-density regions of the cloud. We then use the polarization data at 850 μm to infer the planeof-sky orientation of the large-scale magnetic field in Barnard1. This magnetic field runs north-south across most of the cloud, with the exception of B1-c, where it turns more east-west. From the dispersion of polarization angles, we calculate a turbulence correlation length of 5.0±2 5 (1500 au) and a turbulent-to-total magnetic energy ratio of 0.5±0.3 inside the cloud. We combine this turbulent-to-total magnetic energy ratio with observations of NH 3 molecular lines from the Green Bank Ammonia Survey to estimate the strength of the plane-of-sky component of the magnetic field through the Davis-Chandrasekhar-Fermi method. With a plane-of-sky amplitude of 120±60 μG and a criticality criterion λ c =3.0±1.5, we find that Barnard1 is a supercritical molecular cloud with a magnetic field nearly dominated by its turbulent component.

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Section: Polarization Fraction and Grain Alignmentmentioning

confidence: 72%

The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-forming Region

Coudé¹,

Bastien²,

Houde³

et al. 2019

ApJ

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“…This effect likely decreased our S values compared to Planck Collaboration XIX ( 2015), but Planck Collaboration XX et al (2015) uses the same resolution of 15 as ours, and a very comparable lag scale of = 16 . This means that the difference in S values between our study and those of Planck Collaboration XX et al (2015) will be almost entirely due to the differences in masking.…”

Section: Comparison Of Polarization Propertiesmentioning

confidence: 50%

Characterizing the magnetic fields of nearby molecular clouds using submillimeter polarization observations

Sullivan

Fissel

King

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Of all the factors that influence star formation, magnetic fields are perhaps the least well understood. The goal of this paper is to characterize the 3D magnetic field properties of nearby molecular clouds through various methods of statistically analyzing maps of polarized dust emission. Our study focuses on nine clouds, with data taken from the Planck Sky Survey as well as data from the BLASTPol observations of Vela C. We compare the distributions of polarization fraction (p), dispersion in polarization angles ($\mathcal {S}$), and hydrogen column density (NH) for each of our targeted clouds. To broaden the scope of our analysis, we compare the distributions of our clouds’ polarization observables with measurements from synthetic polarization maps generated from numerical simulations. We also use the distribution of polarization fraction measurements to estimate the inclination angle of each cloud’s cloud-scale magnetic field. We obtain a range of inclination angles associated with our clouds, varying from 16○ to 69○. We establish inverse correlations between p and both $\mathcal {S}$ and NH in almost every cloud, but we are unable to establish a statistically robust $\mathcal {S}$ versus NH trend. By comparing the results of these different statistical analysis techniques, we are able to propose a more comprehensive view of each cloud’s 3D magnetic field properties. These detailed cloud analyses will be useful in the continued studies of cloud-scale magnetic fields and the ways in which they affect star formation within these molecular clouds.

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“…Magnetic field splits into the MFTs due to the Parker (1979) instability in the regions where Bt becomes larger than Bz. We assume that MFTs have the form of the torus with minor radius a mft << H and major radius ac ∼ r.…”

Section: The Stationary Velocity Of the Magnetic Flux Buoyancymentioning

confidence: 99%

“…Ohmic diffusion (OD) and magnetic ambipolar diffusion (MAD) are the main processes that constraint the generation of the magnetic field during the star and disc formation. OD of the magnetic field is caused by currents dissipation in gas with finite conductivity (see Parker (1979)). MAD is the process of plasma drift through the neutral gas under the action of the electromagnetic force.…”

Section: Introductionmentioning

confidence: 99%

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Large-scale magnetic field in the accretion discs of young stars: the influence of magnetic diffusion, buoyancy and Hall effect

Khaibrakhmanov

Dudorov

Parfenov

et al. 2016

Mon. Not. R. Astron. Soc.

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We investigate the fossil magnetic field in the accretion and protoplanetary discs using the Shakura and Sunyaev approach. The distinguishing feature of this study is the accurate solution of the ionization balance equations and the induction equation with Ohmic diffusion, magnetic ambipolar diffusion, buoyancy and the Hall effect. We consider the ionization by cosmic rays, X-rays and radionuclides, radiative recombinations, recombinations onto dust grains, and also thermal ionization. The buoyancy appears as the additional mechanism of magnetic flux escape in the steady-state solution of the induction equation. Calculations show that Ohmic diffusion and magnetic ambipolar diffusion constraint the generation of the magnetic field inside the 'dead' zones. The magnetic field in these regions is quasi-vertical. The buoyancy constraints the toroidal magnetic field strength close to the disc inner edge. As a result, the toroidal and vertical magnetic fields become comparable. The Hall effect is important in the regions close to the borders of the 'dead' zones because electrons are magnetized there. The magnetic field in these regions is quasi-radial. We calculate the magnetic field strength and geometry for the discs with accretion rates (10 −8 −10 −6 ) M ⊙ yr −1 . The fossil magnetic field geometry does not change significantly during the disc evolution while the accretion rate decreases. We construct the synthetic maps of dust emission polarized due to the dust grain alignment by the magnetic field. In the polarization maps, the 'dead' zones appear as the regions with the reduced values of polarization degree in comparison to those in the adjacent regions.

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Planckintermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

Cited by 124 publications

References 50 publications

The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-forming Region

The JCMT BISTRO Survey: The Magnetic Field of the Barnard 1 Star-forming Region

Characterizing the magnetic fields of nearby molecular clouds using submillimeter polarization observations

Large-scale magnetic field in the accretion discs of young stars: the influence of magnetic diffusion, buoyancy and Hall effect

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