On the Magnetic Field Properties of Protostellar Envelopes in Orion

Huang 黄, Bo 博; Girart, Josep M.; Stephens, Ian W.; Fernández López, Manuel; Arce, Hector G.; Carpenter, John M.; Cortes, Paulo; Cox, Erin G.; Friesen, Rachel; Le Gouellec, Valentin J. M.; Hull, Charles L. H.; Karnath, Nicole; Kwon, Woojin; Li, Zhi-Yun; Looney, Leslie W.; Megeath, S. Thomas; Myers, Philip C.; Murillo, Nadia M.; Pineda, Jaime E.; Sadavoy, Sarah; Sánchez-Monge, Álvaro; Sanhueza, Patricio; Tobin, John J.; Zhang, Qizhou; Jackson, James M.; Segura-Cox, Dominique

doi:10.3847/2041-8213/ad27d4

Cited by 3 publications

(2 citation statements)

References 74 publications

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“…This is in contrast to the average magnetic field from the POL-2 and ALMA observations, which are approximately perpendicular to the E-W outflow. On the other hand, this is consistent with the Huang et al (2024) survey, where ∼40% of the sources have average magnetic fields perpendicular to the source outflow.…”

Section: Magnetic Fieldssupporting

confidence: 89%

“…On the other hand, there have been a few surveys of the magnetic field in the inner envelope of protostars comparing the average B-field axis with the outflow axis (Hull et al 2014;Zhang et al 2014;Galametz et al 2018). Most recently, Huang et al (2024) surveyed 61 protostars in Orion (with 56 detections) from the Class 0/I identified disk sources in the VANDAM survey (Tobin et al 2022). They found that ∼40% of the protostars exhibit B-fields that are perpendicular to the source outflows on scales of 400-1000 au, with the remainder of the sources being consistent with random alignment.…”

Section: Introductionmentioning

confidence: 99%

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Magnetic Fields Observed along the East–West Outflow of IRAS 16293-2422

Encalada,

Looney,

Novak

et al. 2024

ApJ

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Magnetic fields likely play an important role in the formation of young protostars. Multiscale and multiwavelength dust polarization observations can reveal the inferred magnetic field from scales of the cloud to core to protostar. We present continuum polarization observations of the young protostellar triple system IRAS 16293-2422 at 89 μm using HAWC+ on SOFIA. The inferred magnetic field is very uniform with an average field angle of 89° ± 23° (E of N), which is different from the ∼170° field morphology seen at 850 μm at larger scales (≳2000 au) with JCMT POL-2 and at 1.3 mm on smaller scales (≲300 au) with Atacama Large Millimeter/submillimeter Array. The HAWC+ magnetic field direction is aligned with the known E-W outflow. This alignment difference suggests that the shorter wavelength HAWC+ data is tracing the magnetic field associated with warmer dust likely from the outflow cavity, whereas the longer wavelength data are tracing the bulk magnetic field from cooler dust. Also, we show in this source the dust emission peak is strongly affected by the observing wavelength. The dust continuum peaks closer to source B (northern source) at shorter wavelengths and progressively moves toward the southern A source with increasing wavelength (from 22 to 850 μm).

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Section: Magnetic Fieldssupporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

Magnetic Fields Observed along the East–West Outflow of IRAS 16293-2422

Encalada,

Looney,

Novak

et al. 2024

ApJ

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Signatures of magnetic braking in Class 0 protostars: Exploring the gas kinematics in magnetized models of low-mass star formation

Añez-López,

Lebreuilly,

Maury

et al. 2024

A&A

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Only indirect evidence of the role of magnetic braking in regulating gravitational collapse and the formation of circumstellar disks, such as compact disk sizes and the launching of high-velocity collimated protostellar jets, has been found from observational work. More direct tests of the magnetic braking shaping the angular momentum of the gas in Class 0 protostars are crucially needed to confirm and make progress on the magnetically regulated disk formation scenario. In the present work we used nonideal magnetohydrodynamic (MHD) models of protostellar collapse and synthetic observations of molecular gas spectral emission, from the radiative transfer post-processing of these models. We analyzed the synthetic observations to test whether possible kinematic signatures of the magnetic braking in the gas velocity field can be captured from maps of the molecular gas emission in protostellar envelopes. By comparing the 3D specific angular momentum of models with varying turbulent energy and magnetization, we show that, in the numerical models of protostellar evolution explored, the increase in magnetization and its consequences on the spatial redistribution of angular momentum modifies the shapes of the radial profiles of specific angular momentum probed along the equatorial plane. However, various analysis of gas kinematics from the synthetic observations of molecular line emission mostly fail to capture the magnitude and differences in radial profiles of specific angular momentum due to different magnetization. Finally, we compare our synthetic observations to observational datasets from the literature to discuss possible magnetic braking signatures in protostellar envelopes. We show that widely used observational methods fail to quantitatively capture the magnitude of angular momentum of the gas in protostellar envelopes, and that no method makes it possible to measure the differences in radial evolution of angular momentum due to different magnetization at all envelope radii. This is especially true in the more magnetized cases where the rotational velocities are of the order of the thermal broadening of the molecular lines. However, our analysis suggests that the detection of symmetric patterns and organized velocity fields in the moment 1 maps of the molecular line emission, and monotonous radial profiles of the specific angular momentum showing a power law decline, should be suggestive of a less magnetized scenario. Protostellar cores where efficient magnetic braking is at work are more likely to present a highly asymmetric velocity field, and more prone to show complex radial profiles of their specific angular momentum measured in the equatorial plane.

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Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46–0.16 Using ALMA

Saha,

Sanhueza,

Padovani

et al. 2024

ApJL

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The contribution of the magnetic field to the formation of high-mass stars is poorly understood. We report the high angular resolution (∼0.″3, 870 au) map of the magnetic field projected on the plane of the sky (B POS) toward the high-mass star-forming region G333.46−0.16 (G333), obtained with the Atacama Large Millimeter/submillimeter Array at 1.2 mm as part of the Magnetic fields in Massive star-forming Regions survey. The B POS morphology found in this region is consistent with a canonical “hourglass” with an embedded flattened envelope in a perpendicular direction, which suggests a dynamically important field. This region is fragmented into two protostars that appear to be gravitationally bound in a stable binary system with a separation of ∼1740 au. Interestingly, by analyzing H13CO+ (J = 3–2) line emission, we find no velocity gradient over the extent of the continuum, which is consistent with a strong field. We model the B POS, obtaining a marginally supercritical mass-to-flux ratio of 1.43, suggesting an initially strongly magnetized environment. Based on the Davis–Chandrasekhar–Fermi method, the magnetic field strength toward G333 is estimated to be 5.7 mG. The absence of strong rotation and outflows toward the central region of G333 suggests strong magnetic braking, consistent with a highly magnetized environment. Our study shows that despite being a strong regulator, the magnetic energy fails to prevent the process of fragmentation, as revealed by the formation of the two protostars in the central region.

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On the Magnetic Field Properties of Protostellar Envelopes in Orion

Cited by 3 publications

References 74 publications

Magnetic Fields Observed along the East–West Outflow of IRAS 16293-2422

Magnetic Fields Observed along the East–West Outflow of IRAS 16293-2422

Signatures of magnetic braking in Class 0 protostars: Exploring the gas kinematics in magnetized models of low-mass star formation

Magnetic Fields in Massive Star-forming Regions (MagMaR): Unveiling an Hourglass Magnetic Field in G333.46–0.16 Using ALMA

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